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a r X i v :a s t r o -p h /0308087v 1 6 A u g 2003
Astronomy &Astrophysics manuscript no.zickgraf February 2,2008
(DOI:will be inserted by hand later)
Kinematical structure of the circumstellar environments of
galactic B[e]-type stars ?
F.-J.Zickgraf
Hamburger Sternwarte,Gojenbergsweg 112,21029Hamburg,Germany
Received date;accepted date
Abstract.High resolution line pro?les are presented for selected forbidden and permitted emission lines of a sample of galactic B[e]-type stars.The spectral resolution corresponds to 5-7km s ?1with the exception of some line pro?les which were observed with a resolution of 9-13km s ?1.All H αpro?les are characterized by a narrow split or single emission component with a width of ～150?250km s ?1(FWHM)and broad wings with a full width of ～1000?2000km s ?1.The H αpro?les can be classi?ed into three groups:double-peaked pro?les representing the majority,single-peaked emission-line pro?les,and normal P Cygni-type pro?les.Likewise,the forbidden lines exhibit in most cases double-peaked pro?les.In particular,the majority of stars
shows split [O I ]λ6300?A.
Double-peaked pro?les are also found in several stars for [N II ]λ6583?A and [Fe II ]λ7155?A although these lines in many stars exhibit single-peaked emission pro?les.The split forbidden line pro?les have peak separations of as little as ～10km s ?1,and were therefore only discernible for the ?rst time in the high-resolution spectra.The ratio of violet to red emission peak intensities,V /R ,is predominantly smaller or equal to 1.Theoretical pro?les were calculated for the optically thin case.A latitude-dependent stellar wind with a radial expansion and a velocity decreasing from the pole to the equator was adopted.This con?guration can produce split line pro?les if viewed under some angle with respect to the line of sight.In addition an equatorial dust ring with various optical depths was assumed.It can explain line asymmetries observed in some stars.Moreover,the V /R ratios can be understood in terms of this model.The comparison of the observed line pro?les with the models thus con?rms the assumption of disk-like line-formation regions as commonly adopted for B[e]-type stars.Key words.Stars:circumstellar matter –Stars:early-type –Stars:emission-line,Be –Stars:mass-loss
1.Introduction
The class of B[e]-type stars is characterized by the B[e]phe-nomenon (Lamers et al.1998).This term summarizes the pres-ence of strong Balmer emission lines,narrow permitted and forbidden low-excitation emission lines of Fe II ,[Fe II ]and [O I ],and in particular a strong near to mid-IR excess.It is attributed to hot circumstellar dust (T dust ～1000K)and is a distinguishing characteristic with respect to other classes of peculiar emission-line stars.The presence of dust requires re-gions of high density and a temperature low enough to allow dust condensation.A recent review of the properties of this still enigmatic class of emission-line stars was given by Zickgraf (1998)during the ?rst workshop dedicated entirely to this type of stars (Hubert &Jaschek 1998).It was shown that although B[e]-type stars share the mentioned properties,indicating very similar physical conditions in their circumstellar environments with regard to temperature,density,and velocity,they form by
2 F.-J.Zickgraf:Circumstellar environments of galactic B[e]-type stars
in the Magellanic Clouds(MCs).These observations strongly suggested that the stellar winds can be described by a two-component model.In this picture a cool and dense equatorial wind emerging from a single star is responsible for the for-mation of the narrow low-excitation emission lines.It is also supposed to be the site of dust formation.The polar region is dominated by a hot and fast expanding OB star wind with the high wind velocities observed normally for stars of this type.
A similar model had been proposed earlier by Swings(1973a) for the galactic B[e]-type star HD45677also based on spectro-scopic observations.In contrast to the post-main sequence MC sgB[e]s it seems to be a(near)main-sequence object.Likewise, the pre-main sequence Herbig Ae/Be stars are supposed to pos-sess circumstellar disks.
Disk-like circumstellar environments could also be caused by binarity.Apart from objects belonging to the subclass of symB[e]several B[e]stars have in fact been shown to be com-ponents of a binary system.In the SMC two B[e]supergiants, Hen S18and R4,were found to possess lower mass com-panions(Zickgraf et al.1989,1996).Likewise,in the Milky Way a couple of B[e]stars were found to be binaries,e.g. MWC623(Zickgraf&Stahl1989),AS381(Miroshnichenko et al.2002a),and CI Cam(=MWC84).Further instances are possibly MWC349A(Hofmann et al.2002)and MWC342 (Miroshnichenko&Corporon1999).It is,however,not clear whether in these objects the B[e]phenomenon itself is actually caused by their binary nature.For some objects this seems not to be the case.In Hen S18,R4,and MWC623the B[e]phe-nomenon can be ascribed to the B star component in the binary systems.These B[e]stars behave like single stars(Zickgraf et al.1989,1996,Zickgraf2001).AS381on the other hand shows signs of mass transfer suggesting that interaction could play a role in the occurence of the B[e]phenomenon in this object(Miroshnichenko et al.2002a).At this time the role of binarity is thus controversial.
Spectroscopic studies showed that the low-excitation lines attributed to the disks are narrow and thus indicative for low wind velocities in the line forming region.Typically, line widths(FWHM)of the order of less than～100km s?1 to300km s?1are observed(e.g.Swings&Andrillat1981, Zickgraf et al.1986).Given the early spectral types of the un-derlying stars such small wind velocities are unusual.
In the case of stars viewed edge-on the direct investiga-tion of the velocity structure of the disk winds is possible by studying absorption lines formed in the disk.This method was used by Zickgraf et al.(1996)to study three B[e]supergiants in the MCs using satellite UV spectroscopy.The observations of UV resonance lines showed that the disk winds are in fact very slow,at least in the case of massive supergiants.The expansion velocities measured were of the order of70-100km s?1,i.e. typically a factor of10less than usually observed for stars of similar spectral type.This may also hold for members of other B[e]star classes.
For viewing angles deviating from edge-on one can make use of the low-excitation emission lines to study the kinematics of the disk winds.Of particular interest are lines from forbidden transitions because they are optically thin.Therefore radiation transfer does not complicate the interpretation of the line in-Table1.Observed sample of B[e]-type stars.References for
spectral types are:WS85=Wolf&Stahl(1985),McG88= McGregor et al.(1988),WW89=Winkler&Wolf(1989), LeB89=Le Bertre et al.(1989),Th′e94=Th′e et al.(1994), Sw73=Swings(1973a),C99=Clark et al.(1999),Lei77= Leibowitz1977),L98=Lamers et al.(1998),Isr96=Israelian et al.(1996),Drew97=Drew et al.(1997).
star spec.class.references tensities and pro?les.Furthermore,the forbidden lines should form at a large distance from the central star.Hence,in the case of a radially accelerated out?ow(as e.g.the usually adopted β-type velocity law)the radial velocity component in the line forming region should have reached the terminal wind speed. Because of the small velocities involved the investigation of the emission-line pro?les requires high spectral resolution.If one aims at a resolution of about1/10of the terminal velocity a spectral resolution of about～5?10km s?1is necessary for the wind velocities measured e.g.by Zickgraf et al.(1996)for
B[e]supergiants.
In order to study the disk winds using emission-line pro-?les a sample of galactic B[e]-type stars listed in Table1was observed with high spectral resolution.In Sect.2the observa-tions are described.The observed line pro?les are described in Sect.3.The density conditions in the line formation region of the forbidden lines are discussed in Sect.4.The role of rotation and expansion is investigated in Sect.5.In Sect.6model cal-culations of optically thin line pro?les are presented and com-pared with the observed lines.Finally,conclusions are given in Sect.7.The Appendix contains the observational data in Sects.
A and B,and remarks on individual stars in Sect.C.An atlas of the high-resolution spectra is presented in Sect.D1.
F.-J.Zickgraf:Circumstellar environments of galactic B[e]-type stars3 Table3.Lines observed with CES in1986(+)and in1988(×).
star Hα+[N II][O I][Fe II][Fe II]Fe II Fe II He I+Na I D
λ6300?Aλ7155?Aλ4287?Aλ6456?Aλ4549/56?Aλ5876?A
Table4.Lines observed at Calar Alto Observatory.Coud′e observations with a resolution of45000are indicated by the letter”h”, coud′e observations obtained with the lower resolution of23000are indicated by”m”.Supplementary observations with FOCES are denoted by the letter“F”.
star Hα+[N II][N II][O I][Fe II]He I+Na I D He I
λ6583?Aλ6300?Aλ7155?Aλ5876?A&λ6678?A
2.Observations and data reduction
The spectroscopic observations were carried out in1986and
1988with the Coud′e Echelle Spectrometer(CES)at the1.4m
CAT at ESO,La Silla,and in1987with the coud′e spec-
trograph at the2.2m telescope at the Centro Astronomico
Hispano Aleman(CAHA)on Calar Alto,Spain.For a few
stars with incomplete coud′e data the observations were sup-
plemented by echelle spectra obtained with FOCES at Calar
Alto Observatory in June2000and February2002.The journal
of observations is given in Table2.
Due to the small spectral coverage of about?30?60?A
provided by the coud′e spectrographs strong emission lines
characteristic for B[e]-type stars were selected and the ob-
served wavelength ranges adjusted around these lines.In Tabs.
3and4the observed lines are listed for each studied object.
During the1987observing run on Calar Alto the northern B[e]-
type star MWC623was included in the sample.The results
on this star have been presented already by Zickgraf&Stahl
(1989)and Zickgraf(2001)and are therefore omitted here.
The CES spectra were collected during two campaigns in
November1986and March1988.The short camera of the
spectrograph was equipped with a RCA CCD(ESO CCD#8,
4 F.-J.Zickgraf:Circumstellar environments of galactic B[e]-type stars
Table2.Journal of observations.
date wavel.range spectral res.instrument
[?A]R=λ/?λ
chip with24μm pixel size.With a diaphragm diameter of 200μm and an entrance slit width of180μm a spectral resolu-tion of34000was achieved,i.e.9km s?1.A full discussion of the FOCES spectra will be given elsewhere(Zickgraf2003,in preparation).Here only the lines observed also with the coud′e spectrographs will be considered.
During all observing campaigns wavelength calibration was obtained with Th-Ar lamps.For?at?elding built-in lamps were used.The coud′e spectra were reduced by application of standard procedures(bias subtraction,?at-?elding,wavelength calibration,normalization)of the ESO-MIDAS image process-ing software package,context longslit.For the FOCES data the ESO-MIDAS context echelle was used.All spectra were?nally rebinned to heliocentric wavelengths.
The spectra in the red spectral region are strongly affected by narrow telluric absorption features.To correct for these lines,the normalized spectra were divided by the normalized spectrum of a hot comparison star with a line free continuum or with possible photospheric lines removed during the normal-ization procedure.For the Hαlines the correction spectrum was created from the object spectra themselves.First each spec-trum was smoothed.Then the original spectrum was divided by the smoothed spectrum.The?nal correction spectrum was then created by averaging several of these individual spectra observed during the same night as the spectrum to be corrected.
The observed spectral sections are displayed in the Appendix in Figs.D.1to D.8together with remarks on the in-dividual objects in Sect.C.For Hαsee Fig.1.3.Observed line pro?les
In the following the observed characteristics of the line pro?les are summarized.Table A.1in the Appendix lists relevant line parameters.Measurements of heliocentric radial velocities are also listed in the Appendix in Table B.1.The pro?les of Hα, of He I emission lines,and of the forbidden lines rebinned on a velocity scale are displayed in Figs.13and2a,b.
The line pro?les can be categorized into four groups:
–group1:normal P Cygni-type line pro?les with an absorp-tion component reaching below the continuum on the violet side of the pro?le and an emission component on the red side,
–group2:single-peaked pure emission lines without absorp-tion components,
–group3:double-peaked emission lines with a central or al-most central absorption component,or at least an intensity dip on one of the line?anks,
–group4:absorption lines.
These pro?le groups correspond to Beals types I,V,III,and VII-VIII,respectively,de?ned by Beals(1955).The pro?le types of the observed lines are summarized in Table5.
3.1.Hαpro?les
A general characteristic of all Hαpro?les displayed in Fig.1is that they exhibit a narrow single or split emission component with a full width at half maximum(FWHM)of about3-5?A, i.e.～150?250km s?1,and broad wings on both sides of the emission component extending up to typically～20?25?A,i.e.～1000km s?1.These wings are generally ascribed to electron scattering(e.g.Zickgraf et al.1986).
Only one star,CPD?52?9243,shows a P Cygni pro?le which resembles the“normal”(group1)pro?le type.Hen485 in1988and MWC1055may also be classed with group1,al-though the absorption components do not reach below the con-tinuum level.
The Hαpro?les of four stars,MWC84,MWC137, MWC297,and Hen230,fall into group2,which exhibits pure emission line pro?les.The FWHM is of the order of3-5?A. Note,however,that the lines are not symmetric.The asymme-try is particularly pronounced in the case of MWC84.
Most of the investigated stars belong to group3exhibiting double-peaked Hαemission lines.In all of the eleven cases of this group the blue emission peak is weaker than the red peak. In no case the central absorption components reaches below the continuum level.For the peculiar line pro?les of HD45677and MWC645see Sect.C.
For several stars Hαwas observed more than once.The pro?les are plotted in Fig.1:MWC137in1987(solid line) and in2002(dashed line);MWC342in1987(solid line)and in2000(dashed line);MWC939in1987(solid line)and1988 (dashed line),the pro?le observed in2000is indistinguish-able that of1988;MWC1055in1987(solid line)and2000 (dashed line);HD87643in1986(solid line)and1988(dashed line);Hen485in1986(solid line)and1988(dashed line).For
Hen485(see text).
malized to the peak?ux.From bottom to top the pro?les of[O I]λ6300A,[Fe II]λ7155A,[N II]λ6583A,and[S III]λ6312A are plotted with shifts in relative intensity of0,0.75,1.5,and2.25,respectively.
the line observed in2002is shown.
3.2.2.[N II]lines
The wavelength region around[N II]λ6583?A is displayed in Fig.D.2.In two stars,CPD?52?9243and HD87643,the [N II]line is absent.The lines visible in the spectra of these stars aroundλ6585?A are probably due to Fe IIλ6586.69?A. Heliocentric radial velocities are v rad=?72km s?1for CPD?52?9243and v rad=?18km s?1for HD87643.In MWC1055[N II]is only weakly discernible.The majority of stars,however,exhibits clearly visible,in many cases strong, [N II]λ6583?A emission.Eight stars show double-peak pro?les. Hen1191shows a sloping line top inclined towards the red side similar to the[O I]line of Hen230,however with a weak peak on the blue edge.Due to this feature the line was classi?ed type 3.Eight stars exhibit single-peaked emission lines.However,in two of these cases,respectively,the pro?les were observed with the lower resolution of23000and34000.They are labelled “e”and”f”in Table5.Note that each of these stars shows a double-peaked(type3)[O I]pro?le.
3.2.3.[Fe II]
The spectral section with[Fe II]λ7155?A is shown in Fig.D.3. Note for that CD?24?5721the forbiddden lines[Fe II]λλ4287, 4276?A were observed instead of the red line(Fig.D.4).In ?ve cases the[Fe II]pro?les are double-peaked similar to[O I]. However,contrary to[O I]the majority of objects,i.e.10,ex-hibits single-peaked pro?les,2of them on a resolution level of 9km s?1.3.2.4.[S III]lines
The[S III]λ6312?A lines are displayed in Fig.D.1.Only four stars exhibit this higher-excitation emission line,i.e.MWC17, MWC84,MWC137,and MWC349A.In MWC137it is very weak and not much can be said about its pro?le.The[S III] line of MWC84is also weak.The strongest[S III]was found in MWC349A.
3.2.5.Fe II lines
For only half of the sample permitted Fe II lines were observed, mostly Fe IIλ6456?A,but also Fe II lines around4550?A for a few stars instead.The wavelength region around Fe IIλ6456?A is displayed in Fig.D.5.Three of the observed stars exhibit single-peak emission lines.Four stars show double-peaked pro-?les.For Hen485the double-peak structure is only weakly in-dicated.CPD?52?9243is the only star showing a P Cygni pro-?le of group1.CD?24?5721is exceptional.This star shows narrow absorption lines(Fig.D.6).The lines identi?ed in the observed spectral sections of this star are listed in Table C.1.
3.2.6.Na I D lines
The lines of the Na I D doublet are shown in Fig.D.7.The spectral section shown in this?gure also contains the line of He Iλ5876?A(see below).Most stars clearly show circumstel-lar Na I emission.Only4of the14observed stars do not show an emission component of the doublet.In most cases the ab-sorption components are blends of multiple narrow absorption
F.-J.Zickgraf:Circumstellar environments of galactic B[e]-type stars9 Table5.Classi?cation of the line pro?le types of the programme stars into groups1to4:1=normal P Cygni pro?le,2=single-peaked emission line,3=double-peaked emission line,4=absorption line.Additional classi?cation codes are:?=weak line, no further classi?cation possible,0=no line visible,–=not observed.For class3a minus or plus sign denotes objects with V/R≤1.0or V/R>1.0,respectively.For Na I D no group is listed because of the confusion due to interstellar absorption components.For this doublet only the presence of emission(“em”)or pure absorption(“abs”)is indicated.
star Hα[O I][Fe II][N II][S III]Fe II He I Na I D
a:Fe IIλ6586c:He Iλ6678in emission
d:He Iλ6678possible blue shifted absorption component
e:observed with R=23000f:observed with FOCES
lines which are very likely mainly due to interstellar absorp-tion.This makes it dif?cult to detect circumstellar absorption features.Because of this problem only the overall appearance of emission or absorption is listed in Table5.Exceptions are CPD?52?9243and possibly Hen485,cf.Sect.C.18and C.14. Heliocentric radial velocities of the absorption components are listed in Table B.2.
3.3.He I lines
The He Iλ5876?A lines are displayed in Fig.D.7.They appear in all four varieties of pro?le types.However,only one star exhibits a clear P Cyg pro?le of type1,namely MWC300.In CPD?57?2874an emission component seems to partly?ll in the absorption component.Two stars show split type3pro?les and?ve stars single-peaked emission pro?les.Six stars show an absorption line.For four stars no observation of He Iλ5876?A were obtained.In MWC137strong variability was found be-tween1987and2002.The He I line changed from absorption to emission(cf.Sect.C.3).
3.4.Summary
An important result of the observations presented here is the detection of one or more double-peaked emission lines in many objects(cf.Table5).Actually,15,possibly16,of the18objects show at least one line with a double-peaked pro?le.This pro?le type is found for both,permitted and forbidden lines,but not necessarily for each line of a particular star.Eleven of the18 objects have split Hαpro?les.Split forbidden lines are found in13objects.Twelve stars exhibit split[O I]lines.The frac-tion of split lines of[N II]and[Fe II]is smaller.Only8of18 stars exhibit split[N II]lines,and5of17stars have split[Fe II] lines.There are only2cases where Hαis double-peaked, but all forbidden lines are single-peaked emission lines.These are HD87643and MWC300.According to Oudmaijer et al. (1998),and Wolf&Stahl(1985and Winkler&Wolf(1989), respectively,they belong to the B[e]supergiants and are most likely viewed under intermediate to pole-on inclination angles. Note,however,that the nature of these stars still is controver-sially discussed(see also Sect.C.5).
A remarkable feature of the double-peaked pro?les is that most,i.e.,～85%,of the observed lines have an intensity ratio of the violet to red component of V/R≤1.Of the43detected type3lines only8show a V/R ratio larger than1.These are 6of26forbidden,and2of16permitted lines(cf.Table A.1). The latter are all Fe II lines.
4.Density conditions in the forbidden-line
forming zone
The interpretation of the observed line pro?les might be com-plicated by the fact that the sample of B[e]-type stars is not ho-mogeneous with respect to the intrinsic object characteristics. The discussion by Lamers et al.(1998)showed that the con-nection between the different classes of B[e]-type stars is the
10 F.-J.Zickgraf:Circumstellar environments of galactic B[e]-type stars
uniformity of the B[e]phenomenon which calls for invoking a common cause for its occurence in different environments.In the following we will therefore take the view of looking primar-ily at the B[e]phenomenon itself rather than at speci?c object classes.
The forbidden-lines in the spectra of B[e]-type stars are dominated by lines of low-excitation ions of neutral or singly ionized metals.Higher excitation lines like [S III ]are rare.This indicates that the temperature
in the
line
emitting
region is about 104K (Lamers et al.1998).The forbidden lines probe the outer low-density zone of the line formation region.A measure for the maximum density in this region is the critical density,N cr ,for which downward collisional and radiative rates are equal.In the approximation of a 2-level ion with upper level u and lower level l it is given by N cr =
A ul
?(u,l )
T
2
(2)
with the collision strength ?(u,l ),the statistical weight g u and
the electron temperature T .According to Viotti (1976)?(u,l )is given by
?(u,l )≈0.2λ4g u A ul
(3)
with the wavelength λin microns.For [Fe II ](14F)λ7155?A
this leads to N cr ?2.2108cm ?3for T e =104K.The critical den-sities are summarized in Table 6.
Table 6.Critical densities,N cr ,of the observed forbidden lines for an electron temperature of T e =104K,and total ion-ization energies,χ,for the production of the respective ion (Cox 2000).The last line gives D 0=N 0/N cr for a density N 0=1011cm ?3at r =1R ?.
ion [O I ]
[Fe II ]
[N II ]
[S III ]
line
λ6300?A
λ7155?A
λ6583?A
λ6312?A
The forbidden lines not only differ with respect to the crit-ical density but also have different ionisation potentials.The
ionisation energy necessary to form Fe II is 7.9eV .For N II an energy of 14.53eV is required.With χ=33.70eV S III has the highest ionisation energy of the observed forbidden lines.Hence,the forbidden lines probe a density interval of about three orders of magnitude,～105-108cm ?3,and a range of ionisation from neutral,[O I ],to [S III ]with an ionisation po-tential of ～34eV .
5.Disk wind:radial expansion vs.rotation
A spherically symmetric and radially expanding wind is ex-pected to form ?at-topped pro?les if the lines are optically thin.This has already been shown by Beals (1931).The forbidden lines in particular form at large distances from the central star where the wind has reached the terminal velocity (see below).A constant velocity wind is expected to form box-shaped lines if the emissivity is constant throughout the emitting volume.
In the observed sample of B[e]-type stars there is just one case,CPD ?57?2874,where a line pro?le comes close to ?at-topped,however not box-shaped.This is the line [O I ]λ6300of this object.The vast majority of the observed pro?les are clearly different from ?at-topped and therefore are inconsis-tent with a spherically symmetric and optically thin line for-mation region.Deviations from ?at-topped pro?les could be produced in the case of spherical symmetry by additional ex-tinction due to dust distributed evenly throughout the line for-mation region.This has been discussed e.g by Appenzeller et al.(1984)for T Tauri stars.However,the pro?le shape expected for this con?guration is not observed in any of the B[e]-type stars of the sample presented here.The polarimetric observa-tions and the forbidden line pro?les therefore strongly indicate that the B[e]phenomenon is correlated with an anisotropic dis-tribution of the circumstellar matter.
Split pro?les of H αsimilar to those shown in Fig.1are fre-quently found in classical Be stars,although the H αequivalent widths in these stars are usually much smaller than in B[e]-type stars and the underlying photospheric absorption component is often discernible.The double-peaked Be star pro?les are gener-ally assigned to a disk-like geometry of the line forming region in connection with rotation.
Mihalas &Conti (1980)discussed the formation of Beals type III,i.e.type 3,line pro?les in the context of the combi-nation of rotation and expansion in a disk-like circumstellar environment.Adding expansion could in particular explain the blueshifted absorption components of H αand the V/R ratios smaller than 1.It would introduce an asymmetry of the line pro?les by shifting the central reversals towards shorter wave-lengths as observed for most B[e]-type stars.For the forbidden lines,however,this mechanism would not work because the lines are optically thin and therefore absorption does not con-tribute.Nevertheless,the combination of expansion and rota-tion could at least explain the observed double-peaked pro?les of H α.
The double-peaked pro?les of the optically thin lines could quite naturally be produced in rotating disks as shown e.g.by P¨o llitsch (1981).Keplerian disks could for example ex-ist around binary B[e]stars (see Sect.1).The pro?les calcu-lated by P¨o llitsch display,however,two emission peaks with
F.-J.Zickgraf:Circumstellar
V/R=1due to the axial symmetry.Pro?les of this type found only in a few cases,e.g.[S III]of MWC349A,[N II] CPD?57?2874,[N II]and[Fe II]of MWC939,and[O I] CD?24?5721and CPD?57?2874.However,the majority double-peak lines has V/R<1including other lines of mentioned stars.It is therefore not obvious that rotation is likely explanation for the double-peaked pro?les.Rather, line pro?les seem to be determined by radial out?ow.
Let us assume as an example a disk-like con?guration
a rotational velocity v0at1R?of v0=300km s?1and constant radial expansion velocity of v exp.Angular
tum conservation requires v rot(r)=v0R?/r.Hence at distance of10R?the rotation velocity would have dropped
ures the solid line designates a ratio of line widths of1.
The observed line widths may help to better understand the possible role of expansion and rotation.In a disk-like circum-stellar environment in which rotation dominates over expansion the forbidden lines are expected to be narrower than the permit-ted lines because the rotational velocity decreases outwards.If rotation is negligible compared to the expansion velocity of a wind accelerated outwards the forbidden lines should have a larger width than the permitted lines.The latter are formed in the accelerating inner wind zone.The forbidden lines originate at large distance from the star where the wind has reached the terminal velocity.
In Figs.5and6the FWHM of[O I]λ6300?A is plotted ver-sus the FWHM of Hαand He I,respectively.They clearly show
The comparison of the line widths of the forbidden lines shown in Fig.7reveals a correlation which is consistent with the assumption that the velocity in the line forming region is constant,and hence that rotation is not important far from the central star.With few exceptions the[O I]line is approx-imately as broad as the[Fe II]line.For[N II]the result is similar,however,with larger scatter.The comparison of[N II] and[Fe II]displayed in the lower left panel of Fig.7shows four stars with broader[Fe II]than[N II].Note that in two of these cases,MWC137and MWC1055,the lines are very weak and the line widths are uncertain.Only Hen485and CPD?57?2874show signi?cantly broader[Fe II]than[N II]. The general trend is towards equal widths or smaller widths for[Fe II].The comparison with[S III]is not meaningful and therefore not shown because only three stars exhibit this line, i.e.MWC17,MWC137,and MWC349A.Inspecting the line
Fig.9.Line splitting of[O I]vs.[N II](left panel)and of[O I] vs.[Fe II](right panel).Upper limits are plotted as arrows. Equal peak separation is represented by the diagonal lines in each panel.
widths listed in Table A.1for[S III]no clear trend emerges for the few lines.
The line splitting is depicted in Figs.8and9.For single lines the velocity corresponding to the spectral resolution was adopted as upper limit of the line splitting.For the line splitting no clear correlation between different lines exists.However, Hαexhibits a much larger splitting than the forbidden metal lines,which is again indicative of a higher velocity in the Hαforming region.A few stars with both,split[Fe II]and[N II] are found close to the diagonal line of equal splitting shown in Fig.9.For[O I]and[N II]the scatter is large.Most upper limits of the line splitting of[N II]λ6583?A are close to the line of equal peak separation.
The line widths are thus consistent with the assumption that in the inner wind zone rotation could play a role.In the outer regions where the forbidden lines are formed a constant veloc-ity wind seems to prevail.
Alternative to rotation,split optically thin emission-line pro?les can result from a radial out?ow with a hollow-cone geometry as discussed e.g.by Appenzeller et al.(1984).Such a con?guration may be considered an approximation of the ra-dially out?owing equatorial disk wind adopted by Zickgraf et al.(1985,1986)for the B[e]supergiants.However,as before the axial symmetry of this con?guration entails the problem of understanding the V/R ratios.In the case of T Tauri stars asymmetric line pro?les were explained e.g by Appenzeller et
(1987)by assuming an opaque
phenomenon is characterized by
dust,a dust disk is also a possible
in B[e]-type stars.As will be
that this disk is opaque.The
a constant velocity law leads
what is observed for the majority
≤1.However,modifying the
pro?les similar to the observed
will be shown in the following
of optically thin lines
wind
thin emission-line pro?les
(1987)(E87hereafter)for the case
stars.They calculated line pro?les
expanding winds with an
forbidden lines of the B[e]-
thin lines were calculated follow-
is shortly summarized here.The
in Fig.5of E87.The requirement
by allowing arbitrary optical depths for an equatorial dust ring(see below).The inclination angle i is measured with respect to the polar axis.Polar coordi-nates r,θ,φof the vector r are de?ned in the stellar reference frame with r being the distance from the star,θthe angle of the vector r with the polar axis andφthe rotation angle around the polar axis.
For the velocity law the latitude-dependent model of E87 was chosen for two reasons.Firstly,it represents a disk-like structure resembling the two-component wind model for B[e] supergiants suggested by Zickgraf et al.(1985)with a fast po-lar and a slow equatorial wind.Secondly,the pro?les for the latitude-independent wind shown in E87do not resemble the observed line pro?les of the B[e]-type stars neither for opti-cally thick nor optically thin dust absorption.
In the latitude-dependent model the wind was chosen to have a constant velocity v(θ)in radial direction depending on the latitudeθaccording to
v(θ)=v max f(θ)(4) with v max being the velocity in polar direction.The latitude-dependent factor f(θ)describes the variation of the wind ve-locity from the pole towards the equator.Assuming e.g.a B supergiant wind in the direction towards the pole with a max-imum expansion velocity of～500?1000km s?1an equa-torial wind velocity of～50?200km s?1would correspond to f(π/2)～0.05?0.25.This assumption is consistent with the equatorial velocities of～100km s?1measured for B[e] supergiants by Zickgraf et al.(1996).
For the model calculations presented below in Figs.10to 14a linear decrease of f(θ)from1to0.2betweenθ=0 andπ/2was adopted.Note that the minimum value of f(π/2)
depths,τ=1000(solid line),τ=1(short dashed line),andτ=0.1(long dashed line).D0and R d were set to1.0and1R?, respectively.The ordinate is the?ux normalized to the maximum.The abscissa is the radial velocity normalized to the maximum wind speed.
speci?es the line width at FWHM.The pro?le shape,however, is independent of this value.The wind velocity was normal-ized to1relative to the velocity in the direction of the polar axis.Other functional dependencies of f(θ)are possible.For example,in the bi-stable wind model suggested by Lamers and Pauldrach(1991)for out?owing disk winds of early-type stars f(θ)could be described by a step or ramp-like function which takes constant values within certain ranges around the equator and the pole with some transition region in between.However, the general characteristics of the pro?les remain similar unless the constant velocity part of the wind prevails.Then the models approach the latitude-independent case.
The electron density N e at point r normalized to the critical density N cr is given by
D e(r,θ,φ)=N e(r,θ,φ)/N cr=D0(R?/r)2v(θ)?1,(5) where D0is the density ratio at r=R?andθ=0.For a given density distribution N e(r)the parameter D0thus depends on the critical density of the line considered.Lower critical density lines correspond to larger D0values.A line with D0=1,1000, or10000has reached the critical density at r=1R?,33R?, or100R?,respectively,in the polar direction.Note that due to the v(θ)dependence the density distribution is disk-like with the density increasing towards the equatorial plane.According to E87the emissivity j(r,θ,φ)for a2-level atom is
j(r,θ,φ)∝D2e[1+D e(δ+1)]?1(6) whereδis the ratio of the collisional rate coef?cients of the lower and upper level.The line pro?les turned out to be insen-sitive toδwhich could therefore be set toδ=0.The emissivity was set to zero for r
v(r,θ,φ)=?v(θ)cosβ(7) with
cosβ=cosθcos i+sinθsin i sinφ,(8)βbeing the angle between r and the line of sight.Finally,the ?ux contributions j(r)?V of all volume elements within r≤r max were summed up in the suitable velocity intervals evenly distributed between?1and+1.
14 F.-J.Zickgraf:Circumstellar
Edwards et al.assumed the presence of an opaque blocking entirely the receding part of the wind.For the stars an equatorial ring structure was adopted instead with inner ring radius R d≥R?and an optical depth ofτd≥The case R d=R?andτd=∞corresponds to the
?guration of E87.The ring structure with R d>R?into account that the inner rim of the dust disk should pend on the dust condensation radius.According to
&Cassinelli(1998)the equilibrium temperature of the varies as T d?T e?(2R d/R?)?2/5.For the B[e]-type stars can therefore be estimated to be～102R?to～2103R?T e?between104K and2.5104K and T d～103K.V elements below the equatorial plane,i.e.atθ>π/2, tribute F d=j(r)?V exp(?τd)to the observed?ux
the line of sight passes through the central hole.In this
F d=F=j(r)?V.Hence,for R d>R?lines with critical densities can be affected differently by the dust
tion because the inner radius of the line-emitting volume,r depends on N cr.
In Figs.10to12the results of the model calculations displayed for the linear f(θ)law and various parameter nations.Figure10shows line pro?les calculated for D0=1. R d=1R?different inclination angles i,and three
of the optical depthτd of0.1,1,and1000.Note that R d=1R?the pro?le shape does not depend on D0.The
?les forτd=1000are identical to those shown by E87. smallerτd leads to a more symmetrical pro?le.For large nation angles double-peaked pro?les are produced.The ratio of the peak?uxes is always≤1and depends onτd. smallτd leads to V/R≈1for all inclination angles.Forτd>～the V/R ratio deviates signi?cantly from1except for large The peak separation is determined by f(θ=π/2)and
also on the inclination i.Decreasing f(θ=π/2)and/or i
a smaller velocity difference of the line peaks.There is some weak dependence of the peak separation onτd.
In Figs.11and12the in?uence of D0as a function of clination is shown for models with a dust ring.The inner
of the ring is assumed to be R d=1000R?.Two sets of
are shown for which the optical depth of the dust isτd=1 1000,respectively.Different D0values were adopted for a lar density at the base of the wind of N0=1011cm?3and critical densities given in Table6for[Fe II],[O I],and[N II This N0corresponds to an equatorial density of～1012cm?For smallτd the pro?les remain nearly symmetric with
ing D0.Only a small decrease of the?ux on the red wing be seen.For intermediate inclination angles the split show a trend of decreasing V/R with increasing D0.For
τd the lines become more asymmetric for increasing D0be-cause the emission for lines with a low critical density starts at a larger distance from the star.Therefore less emission can be seen through the central hole of the dust ring.The con?gura-tion thus approaches that of Fig.10.The receding part of the wind produces a weak bump on the red side of the pro?le if the inclination angles is not too large.For high inclination the V/R ratio decreases with increasing D0,passes through a minimum and then increases again.The models thus show that one line may show V/R≈1and at the same time another line with a different N cr can have V/R<1.dashed line),and1106(long dashed line).For the dust ring an optical depth ofτd=1and an inner radius of R d=1000R?was adopted.
Up to now a disk-like wind model with a latitude-independent ionization structure has been considered. However,lines with different ionization potentials may originate in different zones of the wind.For example,the two-component stellar wind model by Zickgraf et al.(1985) suggests that the cool equatorial zone should give rise to
15
dashed line),and1106(long dashed line).For the dust ring an optical depth ofτd=1000and an inner radius of R d= 1000R?was adopted.
neutral or low-ionisation lines of ions like[O I]and[Fe II]. Lines with higher ionization potential like[N II]and[S III] would originate in hotter yet tenuous regions at higher latitude towards the polar zone.A scenario like this is therefore char-acterized by a latitude-dependent ionization structure.It can be sketched by the hollow and?lled cone model,respectively,
hollow cone geometry
within a certain angle
the?lled cone is
from the polar axis.In the
and“polar cone”will
and?lled cone geometry,
for the case of an opening
plane)for the equa-
(measured from the polar
depth of the dust(τd=1)
are complex.The equa-
to the latitude-independent
(opening angle90?).The
with a decreasing
D0or decreasing
becomes weaker.
in Fig.2and of the
that the general char-
qualitatively be repro-
split or asymmetric
wind model
optical depths.The single
peaks observed for a cou-
inclination angles and
or disk.Furthermore,for a
different critical densities
line pro?les.Likewise,
1to>1are expected if the
e.g.in the equatorial disk
MWC297,MWC349A,
and CPD?52?9243quali-
in Fig.10to12for inter-
In most cases the wings ap-
as expected for a small
are MWC645and
pro?les resemble those for
intermediate inclination.
asymmetry with pro-
In Hen485the[O I]line
also show an asymmetric
645.Line splitting is
of splitting expected for an intermediate inclination could be due to turbulent broaden-ing as discussed below.
The lines of MWC300and HD87643are similar to the pro?les for a small inclination angle and small optical depth of the dust.A near pole-on viewing angle was suggested by Winkler&Wolf(1989)for MWC300and by Oudmaijer et al. (1998)for HD87643.
In Hen1191and CPD?57?2874the[N II]lines are charac-terized by a broad pedestal on top of which a narrow peak is sit-ting.This bears some resemblance with the pro?les calculated
16 F.-J.Zickgraf:Circumstellar environments of galactic B[e]-type stars
for small optical depth of the dust and small to intermediate inclination.
An interesting feature of the polar cone lines shown in Fig. 13and14is that they can have V/R>1if seen under in-termediate to large inclination angle.Neither the models with opening angles of90?displayed in Figs.10to12nor the equatorial disk lines in Figs.13and14show this behaviour. This could explain the[O I]lines in MWC137,MWC342, and CD?24?5721,and the[N II]lines of MWC349A and CPD?57?2874.Likewise,the equatorial disk and polar cone model produces lines with different width,both FWHM and FWZI,which is not the case in the latitude-independent ioniza-tion model.
The complex pro?les obtained for a equatorial disk and polar cone model with optically thin dust were not observed in the sample discussed here.However,the forbidden lines of MWC17and MWC349A show a strong resemblance with the pro?les displayed in Fig.14for optically thick dust and incli-nation i=80?.In both stars the lines of[N II]and[S III]are broader than[O I]and[Fe II].This is expected for the equa-torial disk and polar cone model if the higher ionization lines originate in the polar zone(?lled cone)and the lower ioniza-tion lines in the equatorial region(hollow cone).The pro?les displayed in Fig.11for optically thin dust also exhibit the double peak structure if the inclination is high.However,in these models the line forming regions are not separate for lines with different ionization potential.Contrary to the observa-tions the lines should thus show the same widths.Note that for MWC349A there is observational evidence for the existence of a dust disk seen edge-on(White&Becker1985,Leinert1986, Hofmann et al.2002).The observations are thus in favour of the equatorial disk and polar cone model with optically thick dust.
An interesting feature of this model in the case of large op-tical depth of the dust disk is the behaviour of the V/R ratio. The polar cone line can have a?ux ratio V/R>1and at the same time the corresponding equatorial disk line has V/R<1. This could explain qualitatively the different appearance of the lines in MWC349A which shows simultaneously[O I],[Fe II], and[S III]lines with V/R<1and[N II]with V/R>1.
The equatorial disk and polar cone model also seems promising for MWC137,MWC342,and CD?24?5721.In these objects the[O I]exhibits a V/R ratio>1.In MWC137 the line widths and the V/R ratio suggest that[O I]is a polar cone line,whereas[S III]and[N II]are equatorial disk lines.
In Hen230and MWC1055the[N II]line shows a red wing indicating that this line originates in a polar cone seen under an intermediate aspect angle.In Hen230the wing is also indicated in[Fe II].
Though many line characteristics can thus be understood in terms of the latitude-dependent wind model there seems to be a problem in explaining simultaneously split and single-peaked forbidden lines as observed in several stars.In many of these cases insuf?cient spectral resolution or too low an S/N ratio might be an explanation for the apparent differ-ences of the pro?les,e.g.in MWC297,and MWC1055.In MWC17,MWC342,HD45677,and CD?24?5721,however, the differences seem to be real.A possible explanation could be the existence of macroscopic turbulent motion of the order of～10?30km s?1.It would broaden the local line pro?le and therefore smear out line splitting if the expansion veloc-ities are small enough.As an example a hollow cone model with an opening angle of30?and an inclination angle of45?is shown in Fig.15.For the wind a polar velocity of v max= 300km s?1,and an equatorial velocity of v eq=25km s?1, i.e.f(π/2)=0.08,was adopted.The line broadening due to macro turbulence was assumed to have a Gaussian shape with a FWHM given by the turbulent velocity v t.Four values were as-sumed for v t,i.e.15,20,30,and35km s?1.The optical depth of the dust disk wasτd=1.The?gure shows that the split pro?le disappears for high v t.If the lines originate in differ-ent regions,e.g.due to ionization effects,a location-dependent turbulence velocity could therefore lead to the observed differ-ences in the pro?les.A high v t could also be responsible for the sloping tops of the lines of CPD?52?9243.V/R<1and [N II]with V/R<1(cf.Fig.2).
Alternatively,the simultaneous appearance of split and single-peaked lines of the different ions can be explained with the equatorial disk and polar cone model.MWC342and HD45677show split[O I],but single-peaked[Fe II]and[N II]. Surprisingly,such a combination of pro?les can be produced in a nearly pole-on geometry.This is illustrated in Fig.16for a model with an inclination angle of i=10?.Here it is assumed that the split line originates in the polar cone with a large open-ing angle of about～70?to～80?.The line has a V/R ratio of>1.The single-peaked line is produced with an opening an-gle of90?,which means latitude-independent ionization.This confguration thus can lead to split lines with V/R>1and simultaneously to single-peaked lines.
7.Conclusions
High-resolution line pro?les of selected permitted and forbid-den lines of B[e]-type stars were discussed.A main result was the detection of double-peaked forbidden lines in a large frac-tion of the observed sample.This strongly indicates that the line formation environment has a non-spherical distribution, most likely in a disk-like con?guration.Lines formed close to the star like Hαand He I were compared with forbidden lines formed in the tenuous outskirts.The comparison suggests that rotation could dominate in the inner zones but is overtaken by a radially expanding disk wind in the outer regions.
Line pro?les were calculated for the optically thin case. Pro?les similar to the observed forbidden lines are expected for a radially expanding latitude-dependent wind.This wind con-?guration can be considered a parametrization of the generally accepted two-component wind model for B[e]-type stars.
For many objects in the sample the observed line pro?les are consistent with models assuming a latitude-independent ionization structure of the wind.There are,however,two other groups of objects for which the models suggest(partly)sepa-rated line forming regions for the different ions.In one group the low ionization lines seem to originate in an equatorial disk. In the second group the neutral line of[O I]appears to originate in a polar cone instead.
F.-J.Zickgraf:Circumstellar environments of galactic B[e]-type stars17
It is clear,though,that due to simplifying assumptions of the model it cannot be expected to explain all details of the observed pro?les.Rather,the discrepancies might suggest that the environments,although in general having a disk-like struc-ture,are apparently more complicated than assumed here.In particular,the ionization structure is taken into account only simplistically with the hollow and?lled cone model because of the lack of information on this parameter.For example,charge tranfer reactions can have a strong in?uence on the ioniza-tion balance of oxygen and nitrogen(e.g.Chamberlain1956, Butler&Dalgarno1979).This has not been investigated for B[e]star disks so far.Binarity could add further complexity. However,as long as an expanding wind dominates the circum-stellar environment at large distances from the central object the latitude-dependent wind model could also be applicable to such a subclass of B[e]-type stars.Thus even with the simpli-fying assumptions the results obtained here support the com-monly adopted point of view that the forbidden emission lines of B[e]-type stars are formed in disk-like circumstellar envi-ronments.
Acknowledgements.I would like to thank the Deutsche Forschungs-gemeinschaft for granting travel funds(Zi420/7-1)and for?nancial support under grants Wo269/2-1and Wo269/2-2.I would also like to thank the referee,Dr.A.S.Miroshnichenko,for his critical comments which helped to improve the paper.This research has made use of the SIMBAD database,operated at CDS,Strasbourg,France. References
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Appendix A:Emission line parameters
In Table A.1the line parameters of the observed emission lines listed.Line peak intensities I line=F line/F cont(for the stronger
in case of split pro?les)and the ratio of blue and red peak ties,V/R=(F blue?F cont)/(F red?F cont),are given in the two columns.W is the equivalent width in?A,?v(in km s?1)is peak separation for lines of type3.FWZI and FWHM(in km s?are the full width at zero intensity and full width at half respectively.Errors of FWZI and FWHM were found to be about 15%.The meaning of“FWHM”is taken literally by measuring line widths at the50%?ux level of the maximum peak?ux
dent of the line pro?le shape.For type3pro?les with V/R<0.5 type1P Cygni pro?les this only measures the width of the red sion peak which is then used as a rough estimate for the FWHM. Hαonly a lower limit for FWZI can be given due to the small length intervals covered by the spectra.
Appendix B:Heliocentric radial velocities
In Table B.1heliocentric radial velocities of the different lines listed.For double-peaked emission lines“e b”and“e r”denote the locities of the blue and red emission components,respectively. single-peaked emission lines“c”denotes the velocities of the center emission.In the case of double-peaked lines“c”is the velocity of central absorption or of the central dip between the emission
For pure absorption lines it is the central velocity of the feature.Velocities of absorption components are additionally
by the letter“a”.For type1pro?les absorption velocities are
in the column“e b/a”.The laboratory wavelengths used for the bidden lines are6300.31?A for[O I],7155.14?A for[Fe II],6583.37
for[N II],and6312.10?A for[S III].Table B.2lists the heliocentric dial velocities of the absorption components of the Na I D doublet.In some cases not all components were detectable in each of the doublet components.This is often due to saturation effects in the strong line cores.ometry withτd=1,D0=3105and R d=500R?.For the equatorial disk(solid line)an opening angle of30?measured from the equatorial plane was adopted.The polar cone(dashed line)is the complementary volume with an opening angle of 60?measured from the polar axis.
20 F.-J.Zickgraf:Circumstellar environments of galactic B[e]-type stars Table A.1.Line parameters.
MWC17
Hα180.10.72?680>～205017890 He Iλ5876?A 5.70.68?7.22009754 [O I]λ6300?A25.40.91?27.11035120 [N II]λ6583?A 3.40.92?3.51567016 [Fe II]λ7155?A 3.6–?2.510145–[S III]λ6312?A 3.10.76?3.51397545 line I line V/R W FWZI FWHM?v
MWC137
Hα(1987)86.9–?395>～1400197–Hα(2002)105.3–?464～1600196–He Iλ5876?A(87)––+1.3–––He Iλ5876?A(02) 1.9–?4.1796270–[O I]λ6300?A 1.6 1.20?0.781415829 [Fe II]λ7155?A 1.05–?0.09132:77:–[N II]λ6583?A 1.450.96?0.39953411: [S III]λ6312?A 1.14–?0.106932–line I line V/R W FWZI FWHM?v
MWC300
Hα89.00.38?150>～11406578 He Iλ5876?A 2.10–?1.4120159–[O I]λ6300?A24.5–?10.77521–[N II]λ6583?A 3.1–?1.338825–[Fe II]λ7155?A 1.90–?0.616529–line I line V/R W FWZI FWHM?v line I line V/R W FWZI FWHM?v
MWC645
Hα4780.38?195>～133070188 [O I]λ6300?A10.10.83?14.02797419 [N II]λ6583?A 1.24–?0.3010569–[Fe II]λ7155?A 5.550.82?8.32607026 line I line V/R W FWZI FWHM?v
MWC1055
Hα(1987)680.04?181>～1740101(206) Hα(2000)620.03?1133300113(330) [O I]λ6300?A 2.540.86?0.9054287: [N II]λ6583?A 1.07–?0.0326:13:–[Fe II]λ7155?A 1.11–?0.074726–
Fe IIλ6456?A 1.12–?0.2721899–line I line V/R W FWZI FWHM?v
Hen485
Hα198645.6–?170>～1800159–
Hα198844.70.04:?156>～1830133–
He Iλ5876?A 1.32–?0.92374127–[O I]λ6300?A 1.34–?0.3411641–[N II]λ6583?A(86) 1.67–?0.315322–[N II]λ6583?A(88) 2.86–?0.926222–[Fe II]λ7155?A 1.21–?0.3215345–
Fe IIλ4549?A 2.44–?2.1219885–
首届“教育教学技能大比武”总结 为期半个月的青年教师首届“教育教学技能大比武”活动已经圆满落下帷幕。参加本次比赛的教师都是38周岁以下的青年教师，比赛内容包括讲课、答辩、三笔字、演讲四个环节。这次活动在学校领导的大力支持下，在全体教师的努力配合下，在参赛教师积极参与、认真准备下，取得圆满成功。 回顾本次比赛活动，老师们无论是在个人综合素质、教材把握能力还是在课堂驾驭能力上都有精彩的展示，下面对本次活动做一个总结： 一、讲课赛环节 这十九位青年教师对此次比赛高度重视，认真备课、讲课，为我们呈现了一节节风格各异、亮点纷呈的课，主要呈现了一下几个特点： 1、备课充分、设计用心。 老师们在备课过程中，能深入钻研教材，做了大量充分的准备。老师们都精心设计导语，创设情境，千方百计地激发起学生强烈的求知欲，能够把知识和能力深入浅出又扎扎实实的传授给学生，每一节课都朴实无华，每一节课都独具匠心，比如：郑珊老师在讲授《图形的旋转》一课时，教学设计层次分明，抓住平移和旋转的特征明确其描述方法，在新授的过程中能够放手让学生自己思考-动手操作-小组交流-展示（说明描述），老师引导学生亲历学习过程，通过几个有效的追问，使自己体会掌握了学习内容。 2、教学扎实有效，注重基础训练。 老师们能够抓住教学目标，精心设计每一个环节，同时老师们十分注重基础训练，比如高年级语文老师在教学中注重字词的品读与指导，在阅读教学中，老师能通过阅读来领悟文本的内涵，例如王玉英讲述《梅花魂》一课，她更注重引导学生“品词、品句、品读”以此让学生以读明理，以读悟情，通过“品”字让学生真正体会到了外祖父为什么那么珍爱墨梅图，从而理解梅花的品行，上升到中国人的气节。语文中低年级教学中，教师注重字形的书写字文的理解和区别运用，比如赵彤霞老师执教《植物妈妈有办法》一课，能在文中恰到好处的让学生理解“许多”和“许”“多”的区别，并用“纷纷”说一句话。又比如赵志芳执教《秋天的雨》一课中，注重了“爽”字的书写指导，教学中注重句子的训练，让学生练说比喻句。 3、注重学生情感态度和学习习惯的培养。 注重学生情感态度和学习习惯的培养是成为这次比赛课的又一亮点。老师们在教学中，做到自始至终关注学生的情感，营造宽松、民主、和谐的教学气氛，尊重每个学生，积极鼓励他们在学习中的尝试，保护他们的自尊心和积极性。比如吴蕊霞老师的鼓励具有个性化，激励性的语言常挂嘴边，成为学生不断学习、创新不可缺乏的精神动力。同时在教学中注重学习习惯的培养，比如高月枝老师在授课的同时适时对学生进行了课常规的教育，整个一节课，教学秩序井然有序，对于刚上学两个星期的孩子真的很难得。 4、善用多媒体教学。 本次讲课赛几乎所有的老师都制作了精美实用的多媒体课件，追求既生动形象又快捷高效的教学效果。特别是赵丽和龚伟科两位老师用我们上学期培训的知识制作了白板课件。 5、教师素养良好。 通过这次比赛，我们欣喜地看到我校青年教师具备良好的教师基本素质。他们教态大方得体，语言清晰，具有较强的亲和力和应变能力。王敏、陈蓉等老师她们在课堂上文雅得体的教态，丰富的肢体语言以及亲切和蔼的微笑，都给我们留下了深刻的印象，深受学生的喜爱。 针对本次讲课赛反映出的问题，给老师们提出以下建议，跟老师们商榷：1、语文教学中，略读课文的教学教师应大胆放手学生，让学生充分展示自己。有感情的朗读，重在先理解再
教育资料 《短歌行》 《短歌行》赏析(林庚) 曹操这一首《短歌行》是建安时代杰出的名作，它代表着人生的两面，一方面是人生的忧患，一方面是人生的欢乐。而所谓两面也就是人生的全面。整个的人生中自然含有一个生活的态度，这就具体地表现在成为《楚辞》与《诗经》传统的产儿。它一方面不失为《楚辞》中永恒的追求，一方面不失为一个平实的生活表现，因而也就为建安诗坛铺平了道路。 这首诗从“对酒当歌，人生几何”到“但为君故，沉吟至今”，充分表现着《楚辞》里的哀怨。一方面是人生的无常，一方面是永恒的渴望。而“呦呦鹿鸣”以下四句却是尽情的欢乐。你不晓得何以由哀怨这一端忽然会走到欢乐那一端去，转折得天衣无缝，仿佛本来就该是这么一回事似的。这才是真正的人生的感受。这一段如是，下一段也如是。“明明如月，何时可掇?忧从中来，不可断绝。越陌度阡，枉用相存。契阔谈宴，心念旧恩。月明星稀，乌鹊南飞。绕树三匝，何枝可依。”缠绵的情调，把你又带回更深的哀怨中去。但“山不厌高，海不厌深”，终于走入“周公吐哺，天下归心”的结论。上下两段是一个章法，但是你并不觉得重复，你只觉得卷在悲哀与欢乐的旋涡中，不知道什么时候悲哀没有了，变成欢乐，也不知道什么时候欢乐没有了，又变成悲哀，这岂不是一个整个的人生吗?把整个的人生表现在一个刹那的感觉上，又都归于一个最实在的生活上。“我有嘉宾，鼓瑟吹笙”，不正是当时的情景吗?“周公吐哺，天下归心”，不正是当时的信心吗? “青青子衿”到“鼓瑟吹笙”两段连贯之妙，古今无二。《诗经》中现成的句法一变而有了《楚辞》的精神，全在“沉吟至今”的点窜，那是“青青子衿”的更深的解释，《诗经》与《楚辞》因此才有了更深的默契，从《楚辞》又回到《诗经》，这样与《鹿鸣》之诗乃打成一片，这是一个完满的行程，也便是人生旅程的意义。“月明星稀”何以会变成“山不厌高，海不厌深”?几乎更不可解。莫非由于“明月出天山”，“海上生明月”吗?古辞说：“枯桑知天风，海水知天寒”，枯桑何以知天风，因为它高；海水何以知天寒，因为它深。唐人诗“一叶落知天下秋”，我们对于宇宙万有正应该有一个“知”字。然则既然是山，岂可不高?既然是海，岂可不深呢?“并刀如水，吴盐胜雪”，既是刀，就应该雪亮；既是盐，就应该雪白，那么就不必问山与海了。 山海之情，成为漫漫旅程的归宿，这不但是乌鹊南飞，且成为人生的思慕。山既尽其高，海既尽其深。人在其中乃有一颗赤子的心。孟子主尽性，因此养成他浩然之气。天下所以归心，我们乃不觉得是一个夸张。 .
The way 的用法 Ⅰ常见用法： 1)the way+ that 2)the way + in which（最为正式的用法） 3)the way + 省略（最为自然的用法） 举例：I like the way in which he talks. I like the way that he talks. I like the way he talks. Ⅱ习惯用法： 在当代美国英语中，the way用作为副词的对格，“the way+ 从句”实际上相当于一个状语从句来修饰整个句子。 1)The way =as I am talking to you just the way I’d talk to my own child. He did not do it the way his friends did. Most fruits are naturally sweet and we can eat them just the way they are—all we have to do is to clean and peel them. 2）The way= according to the way/ judging from the way The way you answer the question, you are an excellent student. The way most people look at you, you’d think trash man is a monster. 3）The way =how/ how much No one can imagine the way he missed her. 4）The way =because
教师即兴演讲题目之63个话题 来源：思雨教育资源网|教学资源|课件论文|作文作者：无边思雨发表日期：2009-5-30 13:16:19 阅读次数： 910 查看权限：普通文章 1、如何维护班集体荣誉？ 2、如何看待学生时代早恋问题？ 3、成人与成才二者是怎样的关系？结合实例说明自己的观点。 4、不同地域、不同背景、不同习惯的同学之间该如何相处？ 5、怎样面对学习、生活中遇到的挫折？ 6、你最崇拜的人是谁？“名人”还是自己？ 7、你认为我们是否应有感恩之心？感恩于谁？ 8、你希望自己会是怎样一位老师？你会如何教育自己的学生？ 9、“言行、仪表”与个人的发展。 10、如今继续提倡“勤俭、节约”作风是否已过时？ 11、在各种资料、媒体中常讲张扬个性，你认为我们该张扬什么样的个性？ 12、三轮车工人方尚礼自己生活的如乞丐，却将自己蹬车收入的35万多元用来资助失学儿童，当病重时，社会捐助给他治病的钱，也被他捐给了希望工程。你对方尚礼的这种行为有何评述？ 13、电视广告不宜过多 14、保护环境是每个人的责任 15、我中学时代的一个朋友 16、世界需要热心肠 17、向权威挑战 18、2008年的我 19、我爱电视广告 20、我的母亲 21、尊重是孩子成长的基石 22、如何培养学生的好奇心 23、推广普通话 24、“恶语伤人六月寒” 25、我心中的偶像 26、假如我是画家 27、童年趣事 28、珍惜现在 29、我最爱看的电视节目 30、有人认为老师是不断燃烧的蜡烛，你认为呢？ 31、新课程背景下良好师生场的营造。 32、让谐趣幽默走进我们的课堂。 33、阅读教学中如何开展有效的对话教学？ 34、如何正确处理价值取向和个性化阅读的关系？ 35、新课程背景下一堂好课的标准是什么？ 36、“语文教学工具性与人文性统一”的内涵是什么？ 37、如何实践语文教学的人文性和工具性的“统一”？ 38、如何挖掘教材资源，准确选点，扎实训练？
曹操《短歌行【对酒当歌】》原文、翻译、赏析译文 原文 面对美酒应该高歌，人生短促日月如梭。对酒当歌，人生几何？ 好比晨露转瞬即逝，失去的时日实在太多！譬如朝露，去日苦多。 席上歌声激昂慷慨，忧郁长久填满心窝。慨当以慷，忧思难忘。 靠什么来排解忧闷？唯有狂饮方可解脱。何以解忧？唯有杜康。 那穿着青领（周代学士的服装）的学子哟，你们令我朝夕思慕。青青子衿，悠悠我心。 正是因为你们的缘故，我一直低唱着《子衿》歌。但为君故，沉吟至今。 阳光下鹿群呦呦欢鸣，悠然自得啃食在绿坡。呦呦鹿鸣，食野之苹。 一旦四方贤才光临舍下，我将奏瑟吹笙宴请宾客。我有嘉宾，鼓瑟吹笙。 当空悬挂的皓月哟，你运转着，永不停止；明明如月，何时可掇？ 我久蓄于怀的忧愤哟，突然喷涌而出汇成长河。忧从中来，不可断绝。 远方宾客踏着田间小路，一个个屈驾前来探望我。越陌度阡，枉用相存。 彼此久别重逢谈心宴饮，争着将往日的情谊诉说。契阔谈讌，心念旧恩。 明月升起，星星闪烁，一群寻巢乌鹊向南飞去。月明星稀，乌鹊南飞。 绕树飞了三周却没敛绕树三匝，何枝
翅，哪里才有它们栖身之 所？ 可依？ 高山不辞土石才见巍 峨，大海不弃涓流才见壮阔。（比喻用人要“唯才是举”，多多益善。）山不厌高，水不厌深。 只有像周公那样礼待贤 才（周公见到贤才，吐出口 中正在咀嚼的食物，马上接 待。《史记》载周公自谓： “一沐三握发，一饭三吐哺， 犹恐失天下之贤。”），才 能使天下人心都归向我。 周公吐哺，天 赏析 曹操是汉末杰出的政治家、军事家和文学家，他雅好诗章，好作乐府歌辞，今存诗22首，全是乐府诗。曹操的乐府诗多描写他本人的政治主张和统一天下的雄心壮志。如他的《短歌行》，充分表达了诗人求贤若渴以及统一天下的壮志。 《短歌行》是政治性很强的诗作，主要是为曹操当时所实行的政治路线和政策策略服务的，但是作者将政治内容和意义完全熔铸在浓郁的抒情意境之中，全诗充分发挥了诗歌创作的特长，准确而巧妙地运用了比兴手法，寓理于情，以情感人。诗歌无论在思想内容还是在艺术上都取得了极高的成就，语言质朴，立意深远，气势充沛。这首带有建安时代"志深比长""梗概多气"的时代特色的《短歌行》，读后不觉思接千载，荡气回肠，受到强烈的感染。 对酒当歌，人生几何？ 譬如朝露，去日苦多。 慨当以慷，幽思难忘。 何以解忧，唯有杜康。 青青子衿，悠悠我心。 但为君故，沈吟至今。 呦呦鹿鸣，食野之苹。 我有嘉宾，鼓瑟吹笙。 明明如月，何时可掇？ 忧从中来，不可断绝。 越陌度阡，枉用相存。 契阔谈，心念旧恩。 月明星稀，乌鹊南飞， 绕树三匝，何枝可依？ 山不厌高，海不厌深， 周公吐哺，天下归心。 《短歌行》是汉乐府的旧题，属于《相和歌?平调曲》。这就是说它本来是一个乐曲的名称，这种乐曲怎么唱法，现在当然是不知道了。但乐府《相和歌?平调曲》中除了《短歌行》还有《长歌行》，唐代吴兢《乐府古题要解》引证古诗“长歌正激烈”，魏文帝曹丕《燕歌行》“短歌微吟不能长”和晋代傅玄《艳歌行》“咄来长歌续短歌”等句，认为“长歌”、“短
外国文学名著鉴赏期末论文院—系：数学学院 科目：外国文学名著鉴赏（期末论文）班级： 08级数学与应用数学A班 姓名：沈铁 学号： 200805050149 上课时段：周五晚十、十一节课
奋斗了，才有出路 ——读《鲁宾逊漂游记》有感小说《鲁宾逊漂游记》一直深受人们的喜爱。读完这篇小说，使我对人生应该有自己的一个奋斗历程而受益匪浅。当一个人已经处于绝境的时候，还能够满怀信心的去面对和挑战生活，实在是一种可贵的精神。他使我认识到，人无论何时何地，不管遇到多大的困难，都不能被困难所吓倒，我们要勇敢的面对困难，克服困难，始终保持一种积极向上、乐观的心态去面对。在当今社会只有努力去奋斗，才会有自己的出路！ 其实现在的很多人都是那些遇到困难就退缩，不敢勇敢的去面对它。不仅如此，现在很多人都是独生子女，很多家长视子女为掌上明珠，不要说是冒险了，就连小小的家务活也不让孩子做，天天总是说：“我的小宝贝啊，你读好书就行了，其它的爸爸妈妈做就可以了。”读书固然重要，但生活中的小事也不能忽略。想一想，在荒无人烟的孤岛上，如果你连家务活都不会做，你能在那里生存吗？读完这部著作后，我不禁反问自己：“如果我像书中的鲁宾逊那样在大海遭到风暴，我能向他那样与风暴搏斗，最后逃离荒岛得救吗？恐怕我早已经被大海所淹没；如果我漂流到孤岛，能活几天？我又能干些什么？我会劈柴吗？会打猎做饭吗？我连洗洗自己的衣服还笨手笨脚的。”我们应该学习鲁宾逊这种不怕困难的精神，无论何时何地都有坚持地活下去，哪怕只有一线希望也要坚持到底，决不能放弃！我们要像鲁宾
逊那样有志气、有毅力、爱劳动，凭自己的双手创造财富，创造奇迹，取得最后的胜利。这样的例子在我们的生活中屡见不鲜。 《史记》的作者司马迁含冤入狱，可它依然在狱中完成《史记》一书，他之所以能完成此书，靠的也是他心中那顽强的毅力，永不放弃的不断努力的精神。著名作家爱迪生从小就生活在一个贫困的家庭中，可是他从小就表现出了科学方面的天赋。长大后爱迪生着力于电灯的发明与研究，他经过了九百多次的失败，可它依然没有放弃，不断努力，最后终于在第一千次实验中取得了成功。 鲁宾逊在岛上生活了二十八年，他面对了各种各样的困难和挫折，克服了许多常人无法想象的困难，自己动手，丰衣足食，以惊人的毅力，顽强的活了下来。他自从大船失事后，找了一些木材，在岛上盖了一间房屋，为防止野兽，还在房子周围打了木桩，来到荒岛，面对着的首要的就是吃的问题，船上的东西吃完以后，鲁宾逊开始打猎，有时可能会饿肚子，一是他决定播种，几年后他终于可以吃到自己的劳动成果，其实学习也是这样，也有这样一个循序渐进的过程，现在的社会，竞争无处不在，我们要懂得只有付出才会有收获，要勇于付出，在战胜困难的同时不断取得好成绩。要知道只有付出，才会有收获。鲁宾逊在失败后总结教训，终于成果；磨粮食没有石磨，他就用木头代替；没有筛子，就用围巾。鲁宾逊在荒岛上解决了自己的生存难题，面对人生挫折，鲁宾逊的所作所为充分显示了他坚毅的性格和顽强的精神。同样我们在学习上也可以做一些创新，养成一种创新精神，把鲁宾逊在荒岛，不畏艰险，不怕失败挫折，艰苦奋斗的精
The way的用法及其含义（二） 二、the way在句中的语法作用 the way在句中可以作主语、宾语或表语： 1.作主语 The way you are doing it is completely crazy.你这个干法简直发疯。 The way she puts on that accent really irritates me. 她故意操那种口音的样子实在令我恼火。The way she behaved towards him was utterly ruthless. 她对待他真是无情至极。 Words are important, but the way a person stands, folds his or her arms or moves his or her hands can also give us information about his or her feelings. 言语固然重要,但人的站姿,抱臂的方式和手势也回告诉我们他(她)的情感。 2.作宾语 I hate the way she stared at me.我讨厌她盯我看的样子。 We like the way that her hair hangs down.我们喜欢她的头发笔直地垂下来。 You could tell she was foreign by the way she was dressed. 从她的穿著就可以看出她是外国人。 She could not hide her amusement at the way he was dancing. 她见他跳舞的姿势，忍俊不禁。 3.作表语 This is the way the accident happened.这就是事故如何发生的。 Believe it or not, that's the way it is. 信不信由你, 反正事情就是这样。 That's the way I look at it, too. 我也是这么想。 That was the way minority nationalities were treated in old China. 那就是少数民族在旧中
曹操《短歌行》其二翻译及赏析 引导语：曹操(155—220)，字孟德，小名阿瞒，《短歌行 二首》 是曹操以乐府古题创作的两首诗， 第一首诗表达了作者求贤若渴的心 态，第二首诗主要是曹操向内外臣僚及天下表明心迹。 短歌行 其二 曹操 周西伯昌，怀此圣德。 三分天下，而有其二。 修奉贡献，臣节不隆。 崇侯谗之，是以拘系。 后见赦原，赐之斧钺，得使征伐。 为仲尼所称，达及德行， 犹奉事殷，论叙其美。 齐桓之功，为霸之首。 九合诸侯，一匡天下。 一匡天下，不以兵车。 正而不谲，其德传称。 孔子所叹，并称夷吾，民受其恩。 赐与庙胙，命无下拜。 小白不敢尔，天威在颜咫尺。 晋文亦霸，躬奉天王。 受赐圭瓒，钜鬯彤弓， 卢弓矢千，虎贲三百人。 威服诸侯，师之所尊。 八方闻之，名亚齐桓。 翻译 姬昌受封为西伯，具有神智和美德。殷朝土地为三份，他有其中两分。 整治贡品来进奉，不失臣子的职责。只因为崇侯进谗言，而受冤拘禁。 后因为送礼而赦免， 受赐斧钺征伐的权利。 他被孔丘称赞， 品德高尚地位显。 始终臣服殷朝帝王，美名后世流传遍。齐桓公拥周建立功业，存亡继绝为霸 首。
聚合诸侯捍卫中原，匡正天下功业千秋。号令诸侯以匡周室，主要靠的不是 武力。 行为磊落不欺诈，美德流传于身后。孔子赞美齐桓公，也称赞管仲。 百姓深受恩惠，天子赐肉与桓公，命其无拜来接受。桓公称小白不敢，天子 威严就在咫尺前。 晋文公继承来称霸，亲身尊奉周天王。周天子赏赐丰厚，仪式隆重。 接受玉器和美酒，弓矢武士三百名。晋文公声望镇诸侯，从其风者受尊重。 威名八方全传遍，名声仅次于齐桓公。佯称周王巡狩，招其天子到河阳，因 此大众议论纷纷。 赏析 《短歌行》 (“周西伯昌”)主要是曹操向内外臣僚及天下表明心 迹，当他翦灭群凶之际，功高震主之时，正所谓“君子终日乾乾，夕惕若 厉”者，但东吴孙权却瞅准时机竟上表大说天命而称臣，意在促曹操代汉 而使其失去“挟天子以令诸侯”之号召， 故曹操机敏地认识到“ 是儿欲据吾著炉上郁!”故曹操运筹谋略而赋此《短歌行 ·周西伯 昌》。 西伯姬昌在纣朝三分天下有其二的大好形势下， 犹能奉事殷纣， 故孔子盛称 “周之德， 其可谓至德也已矣。 ”但纣王亲信崇侯虎仍不免在纣王前 还要谗毁文王，并拘系于羑里。曹操举此史实，意在表明自己正在克心效法先圣 西伯姬昌，并肯定他的所作所为，谨慎惕惧，向来无愧于献帝之所赏。 并大谈西伯姬昌、齐桓公、晋文公皆曾受命“专使征伐”。而当 今天下时势与当年的西伯、齐桓、晋文之际颇相类似，天子如命他“专使 征伐”以讨不臣，乃英明之举。但他亦效西伯之德，重齐桓之功，戒晋文 之诈。然故作谦恭之辞耳，又谁知岂无更讨封赏之意乎 ?不然建安十八年(公元 213 年)五月献帝下诏曰《册魏公九锡文》，其文曰“朕闻先王并建明德， 胙之以土，分之以民，崇其宠章，备其礼物，所以藩卫王室、左右厥世也。其在 周成，管、蔡不静，惩难念功，乃使邵康公赐齐太公履，东至于海，西至于河， 南至于穆陵，北至于无棣，五侯九伯，实得征之。 世祚太师，以表东海。爰及襄王，亦有楚人不供王职，又命晋文登为侯伯， 锡以二辂、虎贲、斧钺、禾巨 鬯、弓矢，大启南阳，世作盟主。故周室之不坏， 系二国是赖。”又“今以冀州之河东、河内、魏郡、赵国、中山、常 山，巨鹿、安平、甘陵、平原凡十郡，封君为魏公。锡君玄土，苴以白茅，爰契 尔龟。”又“加君九锡，其敬听朕命。” 观汉献帝下诏《册魏公九锡文》全篇，尽叙其功，以为其功高于伊、周，而 其奖却低于齐、晋，故赐爵赐土，又加九锡，奖励空前。但曹操被奖愈高，心内 愈忧。故曹操在曾早在五十六岁写的《让县自明本志令》中谓“或者人见 孤强盛， 又性不信天命之事， 恐私心相评， 言有不逊之志， 妄相忖度， 每用耿耿。
（一）文学常识 一、古希腊罗马 1．（1）宙斯(罗马神话称为朱庇特)，希腊神话中最高的天神，掌管雷电云雨，是人和神的主宰。 （2）阿波罗，希腊神话中宙斯的儿子，主管光明、青春、音乐、诗歌等，常以手持弓箭的少年形象出现。 （3）雅典那，希腊神话中的智慧女神，雅典城邦的保护神。 （4）潘多拉，希腊神话中的第一个女人，貌美性诈。私自打开了宙斯送她的一只盒子，里面装的疾病、疯狂、罪恶、嫉妒等祸患，一齐飞出，只有希望留在盒底，人间因此充满灾难。“潘多拉的盒子”成为“祸灾的来源”的同义语。 （5）普罗米修斯，希腊神话中造福人间的神。盗取天火带到人间，并传授给人类多种手艺，触怒宙斯，被锁在高加索山崖，受神鹰啄食，是一个反抗强暴、不惜为人类牺牲一切的英雄。 （6）斯芬克司，希腊神话中的狮身女怪。常叫过路行人猜谜，猜不出即将行人杀害；后因谜底被俄底浦斯道破，即自杀。后常喻“谜”一样的人物。与埃及狮身人面像同名。 2．荷马，古希腊盲诗人。主要作品有《伊利亚特》和《奥德赛》，被称为荷马史诗。《伊利亚特》叙述十年特洛伊战争。《奥德赛》写特洛伊战争结束后，希腊英雄奥德赛历险回乡的故事。马克思称赞它“显示出永久的魅力”。 3．埃斯库罗斯，古希腊悲剧之父，代表作《被缚的普罗米修斯》。6．阿里斯托芬，古希腊“喜剧之父”代表作《阿卡奈人》。 4．索福克勒斯，古希腊重要悲剧作家，代表作《俄狄浦斯王》。5．欧里庇得斯，古希腊重要悲剧作家，代表作《美狄亚》。 二、中世纪文学 但丁，意大利人，伟大诗人，文艺复兴的先驱。恩格斯称他是“中世纪的最后一位诗人，同时又是新时代的最初一位诗人”。主要作品有叙事长诗《神曲》，由地狱、炼狱、天堂三部分组成。《神曲》以幻想形式，写但丁迷路，被人导引神游三界。在地狱中见到贪官污吏等受着惩罚，在净界中见到贪色贪财等较轻罪人，在天堂里见到殉道者等高贵的灵魂。 三、文艺复兴时期 1．薄迦丘意大利人短篇小说家，著有《十日谈》拉伯雷，法国人，著《巨人传》塞万提斯，西班牙人,著《堂?吉诃德》。 2．莎士比亚，16-17世纪文艺复兴时期英国伟大的剧作家和诗人，主要作品有四大悲剧——《哈姆雷特》、《奥赛罗》《麦克白》、《李尔王》，另有悲剧《罗密欧与朱丽叶》等，喜剧有《威尼斯商人》《第十二夜》《皆大欢喜》等，历史剧有《理查二世》、《亨利四世》等。马克思称之为“人类最伟大的戏剧天才”。 四、17世纪古典主义 9．笛福，17-18世纪英国著名小说家，被誉为“英国和欧洲小说之父”，主要作品《鲁滨逊漂流记》，是英国第一部现实主义长篇小说。10．弥尔顿，17世纪英国诗人，代表作：长诗《失乐园》，《失乐园》，表现了资产阶级清教徒的革命理想和英雄气概。 25．拉伯雷，16世纪法国作家，代表作：长篇小说《巨人传》。 26．莫里哀，法国17世纪古典主义文学最重要的作家，法国古典主义喜剧的创建者，主要作品为《伪君子》《悭吝人》（主人公叫阿巴公）等喜剧。 五、18世纪启蒙运动 1）歌德，德国文学最高成就的代表者。主要作品有书信体小说《少年维特之烦恼》，诗剧《浮士德》。 11．斯威夫特，18世纪英国作家，代表作：《格列佛游记》，以荒诞的情节讽刺了英国现实。 12．亨利·菲尔丁，18世纪英国作家，代表作：《汤姆·琼斯》。 六、19世纪浪漫主义 （1拜伦， 19世纪初期英国伟大的浪漫主义诗人，代表作为诗体小说《唐璜》通过青年贵族唐璜的种种经历，抨击欧洲反动的封建势力。《恰尔德。哈洛尔游记》 （2雨果，伟大作家，欧洲19世纪浪漫主义文学最卓越的代表。主要作品有长篇小说《巴黎圣母院》、《悲惨世界》、《笑面人》、《九三年》等。《悲惨世界》写的是失业短工冉阿让因偷吃一片面包被抓进监狱，后改名换姓，当上企业主和市长，但终不能摆脱迫害的故事。《巴黎圣母院》 弃儿伽西莫多，在一个偶然的场合被副主教克洛德.孚罗洛收养为义子，长大后有让他当上了巴黎圣母院的敲钟人。他虽然十分丑陋而且有多种残疾，心灵却异常高尚纯洁。 长年流浪街头的波希米亚姑娘拉.爱斯梅拉达，能歌善舞，天真貌美而心地淳厚。青年贫诗人尔比埃尔.甘果瓦偶然同她相遇，并在一个更偶然的场合成了她名义上的丈夫。很有名望的副教主本来一向专心于"圣职"，忽然有一天欣赏到波希米亚姑娘的歌舞，忧千方百计要把她据为己有，对她进行了种种威胁甚至陷害，同时还为此不惜玩弄卑鄙手段，去欺骗利用他的义子伽西莫多和学生甘果瓦。眼看无论如何也实现不了占有爱斯梅拉达的罪恶企图，最后竟亲手把那可爱的少女送上了绞刑架。 另一方面，伽西莫多私下也爱慕着波希米亚姑娘。她遭到陷害，被伽西莫多巧计救出，在圣母院一间密室里避难，敲钟人用十分纯朴和真诚的感情去安慰她，保护她。当她再次处于危急中时，敲钟人为了援助她，表现出非凡的英勇和机智。而当他无意中发现自己的"义父"和"恩人"远望着高挂在绞刑架上的波希米亚姑娘而发出恶魔般的狞笑时，伽西莫多立即对那个伪善者下了最后的判决，亲手把克洛德.孚罗洛从高耸入云的钟塔上推下，使他摔的粉身碎骨。 （3司汤达，批判现实主义作家。代表作《红与黑》，写的是不满封建制度的平民青年于连，千方百计向上爬，最终被送上断头台的故事。“红”是将军服色，指“入军界”的道路；“黑”是主教服色，指当神父、主教的道路。 14．雪莱，19世纪积极浪漫主义诗人，欧洲文学史上最早歌颂空想社会主义的诗人之一，主要作品为诗剧《解放了的普罗米修斯》，抒情诗《西风颂》等。 15．托马斯·哈代，19世纪英国作家，代表作：长篇小说《德伯家的苔丝》。 16．萨克雷，19世纪英国作家，代表作：《名利场》 17．盖斯凯尔夫人，19世纪英国作家，代表作：《玛丽·巴顿》。 18．夏洛蒂?勃朗特，19世纪英国女作家，代表作：长篇小说《简?爱》19艾米丽?勃朗特，19世纪英国女作家，夏洛蒂?勃朗特之妹，代表作：长篇小说《呼啸山庄》。 20．狄更斯，19世纪英国批判现实主义文学的重要代表，主要作品为长篇小说《大卫?科波菲尔》、《艰难时世》《双城记》《雾都孤儿》。21．柯南道尔，19世纪英国著名侦探小说家，代表作品侦探小说集《福尔摩斯探案》是世界上最著名的侦探小说。 七、19世纪现实主义 1、巴尔扎克，19世纪上半叶法国和欧洲批判现实主义文学的杰出代表。主要作品有《人间喜剧》，包括《高老头》、《欧也妮·葛朗台》、《贝姨》、《邦斯舅舅》等。《人间喜剧》是世界文学中规模最宏伟的创作之一，也是人类思维劳动最辉煌的成果之一。马克思称其“提供了一部法国社会特别是巴黎上流社会的卓越的现实主义历史”。
定冠词the的用法： 定冠词the与指示代词this ,that同源,有“那(这)个”的意思,但较弱,可以和一个名词连用,来表示某个或某些特定的人或东西. (1)特指双方都明白的人或物 Take the medicine.把药吃了. (2)上文提到过的人或事 He bought a house.他买了幢房子. I've been to the house.我去过那幢房子. (3)指世界上独一无二的事物 the sun ,the sky ,the moon, the earth (4)单数名词连用表示一类事物 the dollar 美元 the fox 狐狸 或与形容词或分词连用,表示一类人 the rich 富人 the living 生者 (5)用在序数词和形容词最高级,及形容词等前面 Where do you live?你住在哪? I live on the second floor.我住在二楼. That's the very thing I've been looking for.那正是我要找的东西. (6)与复数名词连用,指整个群体 They are the teachers of this school.(指全体教师) They are teachers of this school.(指部分教师) (7)表示所有,相当于物主代词,用在表示身体部位的名词前 She caught me by the arm.她抓住了我的手臂. (8)用在某些有普通名词构成的国家名称,机关团体,阶级等专有名词前 the People's Republic of China 中华人民共和国 the United States 美国 (9)用在表示乐器的名词前 She plays the piano.她会弹钢琴. (10)用在姓氏的复数名词之前,表示一家人 the Greens 格林一家人(或格林夫妇) (11)用在惯用语中 in the day, in the morning... the day before yesterday, the next morning... in the sky... in the dark... in the end... on the whole, by the way...
题目：浅析从简爱到女性的尊严和爱 学院工商学院 专业新闻学3 学号 姓名闫万里 学科外国文学名着赏析 [摘要] 十九世纪中期，英国伟大的女性存在主义先驱，着名作家夏洛蒂勃朗特创作出了她的代表作--《简爱》，当时轰动了整个文坛,它是一部具有浓厚浪漫主义色彩的现实主义小说，被认为是作者"诗意的生平"的写照。它在问世后的一百多年里，它始终保持着历史不败的艺术感染力。直到现在它的影响还继续存在。在作品的序幕、发展、高潮和结尾中，女主人公的叛逆、自由、平等、自尊、纯洁的个性都是各个重点章节的主旨，而这些主旨则在女主人公的爱情观中被展露的淋漓尽致，它们如同乌云上方的星汉，灼灼闪耀着光芒，照亮着后来的女性者们追求爱情的道路。? [关键词] 自尊个性独特新女性主义自由独立平等 《简爱》是一部带有自转色彩的长篇小说，它阐释了这样一个主题：人的价值=尊严+爱。从小就成长在一个充满暴力的环境中的简爱，经历了同龄人没有的遭遇。她要面对的是舅妈的毫无人性的虐待，表兄的凶暴专横和表姐的傲慢冷漠，尽管她尽力想“竭力赢得别人的好感”，但是事实告诉她这都是白费力气的，因此她发出了“不公平啊！--不公平！”的近乎绝望的呼喊。不公平的生长环境，使得简爱从小就向往平等、自由和爱，这些愿望在她后来的成长过程中表现无疑，
譬如在她的爱情观中的种种体现。? 1.桑菲尔德府? 谭波儿小姐因为出嫁，离开了洛伍德学校，同时也离开了简爱，这使简爱感觉到了“一种稳定的感觉，一切使我觉得洛伍德学校有点像我家的联想，全都随着她消失了”，她意识到：真正的世界是广阔的，一个充满希望和忧虑、激动和兴奋的变化纷呈的天地，正等待着敢于闯入、甘冒风险寻求人生真谛的人们。意识形态的转变促使着简爱走向更广阔的社会，接受社会的挑战，尽管她才只有十八岁。于是，简爱来到了桑菲尔德府，当了一名在当时地位不高的家庭教师。?桑菲尔德府使简爱感受到“这儿有想象中的完美无缺的家庭安乐气氛”，事实证明了她的预感的正确性，。从和简爱相见、相识到相爱的过程当中，简爱的那种叛逆精神、自强自尊的品质深深地征服了罗切斯特，而罗切斯特的优雅风度和渊博知识同样也征服了简爱。最初开始，简爱一直以为罗切斯特会娶高贵漂亮的英格拉姆为妻，她在和罗切斯特谈到婚姻时，曾经义正言辞的对罗切斯特说：“你以为因为我穷，低微，不美，矮小，就没有灵魂了吗？你想错了！我跟你一样有灵魂—也同样有一颗心！我现在不是凭着肉体凡胎跟你说话，而是我的心灵在和你的心灵说话，就好像我们都已经离开人世，两人平等地站在上帝面前—因为我们本来就是平等的。”这充分表现出简爱的叛逆，她这种维护妇女独立人格、主张婚姻独立自主以及男女平等的主张可以看成是他对整个人类社会自由平等的向往追求，罗切斯特正是爱上了她这样的独特个性，同时他也同样重复道：我们本来就是平等的。罗切斯特自始自终爱的是简爱的心灵—有着意志的力量，美德和纯洁的心灵，正是基于如此，简爱才真正的爱着罗切斯特。因为爱情是来不得半点虚假的，一方为另一方付出了真情的爱，假如得到对方的是虚情假意，那么这份爱
“tｈｅwａｙ+从句”结构的意义及用法 首先让我们来看下面这个句子: Ｒead the foｌloｗｉnｇpassagｅａnd talkａbout ｉt wi ｔh your classmaｔes．Try tｏｔeｌl whaｔyｏu thiｎk ｏf Tom aｎd ｏｆｔhe ｗay the chiｌｄrenｔrｅated ｈim. 在这个句子中，ｔhe waｙ是先行词,后面是省略了关系副词that或in whｉch的定语从句。 下面我们将叙述“the ｗaｙ+从句”结构的用法。 1.tｈe wａy之后，引导定语从句的关系词是tｈat而不是hoｗ,因此，<<现代英语惯用法词典＞＞中所给出的下面两个句子是错误的：Ｔhｉs is ｔｈeｗayｈowｉtｈａppened. This is the way how he ａlwａｙs treats me. 2．在正式语体中,thaｔ可被in which所代替;在非正式语体中，ｔhat则往往省略。由此我们得到theｗay后接定语从句时的三种模式：1) tｈe ｗaｙ＋ｔhａt-从句２）the way +ｉn whiｃh－从句3) the ｗay +从句 例如：Ｔｈe way(in whiｃh ，thａt) ｔhｅｓｅｃomｒade ｓloｏｋａｔｐrobｌems is wrong．这些同志看问题的方法
不对。 Ｔｈｅｗａy(that ,ｉn ｗhiｃh)yoｕ’ｒe doinｇit is comple ｔeｌy crａzy.你这么个干法,简直发疯。 Wｅａdmiｒｅd him for thｅｗay ｉｎｗhｉch he fａｃeｓdiｆficultieｓ． Waｌlａｃe ａｎd Ｄarwiｎｇreed ｏn the way ｉｎwhi ｃh ｄｉfｆｅrｅnt forms ｏf life had ｂegｕn.华莱士和达尔文对不同类型的生物是如何起源的持相同的观点。 Thｉs is ｔｈe ｗaｙ（tｈａｔ) hｅdｉd it. I lｉkeｄｔhe waｙ(ｔhat) ｓｈeｏｒganized ｔhe ｍeetｉng． 3.theｗay(tｈat)有时可以与hｏw(作“如何”解）通用。例如： That’s tｈe ｗaｙ(tｈaｔ) shｅspoke. = Tｈat’s how shｅspoke.
短歌行赏析介绍 说道曹操， 大家一定就联想到三国那些烽火狼烟岁月吧。 但是曹操其实也是 一位文学 大家，今天就来分享《短歌行 》赏析。 《短歌行》短歌行》是汉乐府旧题，属于《相和歌辞·平调曲》。这就是说 它本来是一个乐曲名称。最初古辞已经失传。乐府里收集同名诗有 24 首，最早 是曹操这首。 这种乐曲怎么唱法， 现在当然是不知道。 但乐府 《相和歌·平调曲》 中除《短歌行》还有《长歌行》，唐代吴兢《乐府古题要解》引证古诗 “长歌正激烈”， 魏文帝曹丕 《燕歌行》 “短歌微吟不能长”和晋代傅玄 《艳 歌行》 “咄来长歌续短歌”等句， 认为“长歌”、 “短歌”是指“歌声有长短”。 我们现在也就只能根据这一点点材料来理解《短歌行》音乐特点。《短歌行》这 个乐曲，原来当然也有相应歌辞，就是“乐府古辞”，但这古辞已经失传。现在 所能见到最早《短歌行》就是曹操所作拟乐府《短歌行》。所谓“拟乐府”就是 运用乐府旧曲来补作新词，曹操传世《短歌行》共有两首，这里要介绍是其中第 一首。 这首《短歌行》主题非常明确，就是作者希望有大量人才来为自己所用。曹 操在其政治活动中，为扩大他在庶族地主中统治基础，打击反动世袭豪强势力， 曾大力强调“唯才是举”，为此而先后发布“求贤令”、“举士令”、“求逸才 令”等;而《短歌行》实际上就是一曲“求贤歌”、又正因为运用诗歌 形式，含有丰富抒情成分，所以就能起到独特感染作用，有力地宣传他所坚 持主张，配合他所颁发政令。 《短歌行》原来有“六解”(即六个乐段)，按照诗意分为四节来读。 “对酒当歌，人生几何?譬如朝露，去日苦多。慨当以慷，忧思难忘。何以 解忧，唯有杜康。” 在这八句中，作者强调他非常发愁，愁得不得。那么愁是什么呢?原来他是 苦于得不到众多“贤才”来同他合作， 一道抓紧时间建功立业。 试想连曹操这样 位高权重人居然在那里为“求贤”而发愁， 那该有多大宣传作用。 假如庶族地主 中真有“贤才”话， 看这些话就不能不大受感动和鼓舞。 他们正苦于找不到出路
外国文学名著赏析 ——对《哈姆雷特》与《堂吉诃德》人物形象及其现实意义的 分析 班级：学号：姓名： 摘要：《哈姆雷特》和《堂吉诃德》是文艺复兴时期涌现出来的一批比较先进的文学作品，通过对两部文学作品的阅读，我们不难发现两部作品所展现出来的人物形象都反映出了当时不同的社会现实，而且两部文学作品都表现出了浓厚的人文主义色彩，并且在当时也带来了不同的社会作用。堂吉诃德是塞万提斯塑造的一个为了打击骑士文学的文学形象，作者通过对堂吉诃德的描写，生动的说明了骑士文学给世人带来的负面影响，从而给骑士文学以致命的打击。莎士比亚笔下的哈姆雷特则是一个孤独的人文主义者，他以失败告终，哈姆雷特的失败向人们揭示了人文主义时代的悲剧。 Abstract: Hamlet a nd Don Quixote were the advanced literary in the Renaissance Period .After read the two novels, it is not difficult to find that different characters in these novels reflected different social problems. And they all expressed the ideas of humanism. These two images also brought different social functions at that time .Don Quixote is one of which Cervantes’s molds in order to attack the knight literature .According to the description of Don Quixote, vivid explain ed that knight literature brought a serious of bad influence to the human beings, thus gives the knight literature by the fatal attack. Hamlet is a lonely humanism, he is end in failure .His failure has indicated the tragedy which in the Humanism Era. 关键词：人文主义、哈姆雷特、人物形象、艺术特色、堂吉诃德、现实意义、悲剧 Key words:humanism; Hamlet; characters; art features; Don Quixote; realistic significance; tragedy 前言： 莎士比亚和塞万提斯都是文艺复兴时期伟大的戏剧家，作为戏剧艺术的大师，他们的作品都达到了世界文学的巅峰。《哈姆雷特》是莎士比亚最著名的悲剧之一，代表了莎士比亚的艺术成就，剧中莎士比亚塑造的著名人物哈姆雷特也被列入了世界文学的艺术画廊。塞万提斯是文艺复兴时期西班牙伟大的作家，在他创作的作品中，以《堂吉诃德》最为著名，影响也最大，是文艺
表示“方式”、“方法”，注意以下用法： 1.表示用某种方法或按某种方式，通常用介词in(此介词有时可省略)。如： Do it (in) your own way. 按你自己的方法做吧。 Please do not talk (in) that way. 请不要那样说。 2.表示做某事的方式或方法，其后可接不定式或of doing sth。 如： It’s the best way of studying [to study] English. 这是学习英语的最好方法。 There are different ways to do [of doing] it. 做这事有不同的办法。 3.其后通常可直接跟一个定语从句(不用任何引导词)，也可跟由that 或in which 引导的定语从句，但是其后的从句不能由how 来引导。如： 我不喜欢他说话的态度。 正：I don’t like the way he spoke. 正：I don’t like the way that he spoke. 正：I don’t like the way in which he spoke. 误：I don’t like the way how he spoke. 4.注意以下各句the way 的用法： That’s the way (=how) he spoke. 那就是他说话的方式。 Nobody else loves you the way(=as) I do. 没有人像我这样爱你。 The way (=According as) you are studying now, you won’tmake much progress. 根据你现在学习情况来看，你不会有多大的进步。 2007年陕西省高考英语中有这样一道单项填空题： ——I think he is taking an active part insocial work. ——I agree with you_____. A、in a way B、on the way C、by the way D、in the way 此题答案选A。要想弄清为什么选A，而不选其他几项，则要弄清选项中含way的四个短语的不同意义和用法，下面我们就对此作一归纳和小结。 一、in a way的用法 表示：在一定程度上，从某方面说。如： In a way he was right.在某种程度上他是对的。注：in a way也可说成in one way。 二、on the way的用法 1、表示：即将来(去)，就要来(去)。如： Spring is on the way.春天快到了。 I'd better be on my way soon.我最好还是快点儿走。 Radio forecasts said a sixth-grade wind was on the way.无线电预报说将有六级大风。 2、表示：在路上，在行进中。如： He stopped for breakfast on the way.他中途停下吃早点。 We had some good laughs on the way.我们在路上好好笑了一阵子。 3、表示：(婴儿)尚未出生。如： She has two children with another one on the way.她有两个孩子，现在还怀着一个。 She's got five children，and another one is on the way.她已经有5个孩子了，另一个又快生了。 三、by the way的用法