a r X i v :a s t r o -p h /0407181v 1 8 J u l 2004
Astronomy &Astrophysics manuscript no.February 2,2008
(DOI:will be inserted by hand later)
Super-Eddington accretion rates in Narrow Line Seyfert 1
galaxies
Suzy Collin 1,Toshihiro Kawaguchi 1,2
1LUTH,Observatoire de Paris,Section de Meudon,F-92195Meudon Cedex,France 2
Postdoctoral Fellow of the Japan Society for the Promotion of Science
the date of receipt and acceptance should be inserted later
Abstract.We use the BH masses deduced from the empirical relation of Kaspi et al.(2000)between the size of the Broad Line Region (BLR)of Active Galactic Nuclei (AGN)and the optical luminosity,to compute their accretion rate in four samples of AGN,assuming that the optical luminosity is provided by the accretion disc.We show that Narrow Line Seyfert Galaxies 1(NLS1s)accrete at super-Eddington rates,while their luminosity stays of the order of the Eddington limit.We take into account the possibility of a non-viscous energy release inversely proportional to the square of the distance in the gravitationally unstable region of the disc emitting a fraction of the optical luminosity.It leads to a smaller accretion rate and to a redder continuum than a standard disc,which agrees better with the observations.The observed bolometric luminosities appear to saturate at a few times the Eddington luminosity for super-Eddington accretion rates,as predicted by slim disc models.They favor a Kerr BH rather than a Schwarzshild one.Even when the accretion rate is super-Eddington,it stays always of the order of a few M ⊙/yr,irrespective of the BH mass,indicating that the growing of the BH is mass supply limited and therefore regulated by an exterior mechanism,and not Eddington limited.The mass of the BH increases by one order of magnitude in a few 107years,a time smaller than that necessary for changing the bulge mass.This is in agreement with recent claims that the BHs of NLS1s do not follow the same black hole -bulge relation as other galaxies.Since they represent about 10%of AGN up to a redshift of 0.5,these “super-active”phases should play an important role in shaping the mass function of local BHs.We ?nally discuss the possibility that the masses could be systematically underestimated due to an inclination e?ect,and we conclude that it could indeed be the case,and that the accretion rates could thus be strongly overestimated in a small proportion of objects,possibly explaining the existence of apparently extremely high accretors.
Key words.Quasars:general -Accretion,accretion discs -galaxies:active -galaxies:Seyfert
1.Introduction and rationale
The evolution of massive black holes (BHs)in relation with their host galaxy is presently intensively debated.Massive black holes seem present in all galactic nuclei,in-dependently of their level of activity.In about 40inactive nearby galaxies,their mass was found proportional to the luminosity of the bulge of the host galaxy (Magorrian et al.1988).Ferrarese &Merritt (2000)and Gebhardt et al.(2000a)showed that a tighter relation exists between the mass of the BH,M ,and the dispersion velocity σB of the bulge.The slope of the relation is still debated,and the recent work of Tremaine et al.(2003)gives a value close to 4.Several mechanisms accounting for this relation have been proposed (Silk &Rees 1998,Umemura 2001,King 2003).When σB is expressed in terms of the bulge mass,it leads to M ～0.002M (Bulge).It is thus clear that the growth of the BH and the evolution of the host galaxy are
2Suzy Collin and Toshihiro Kawaguchi:The accretion rate in NLS1s
Broad Emission Line Region(BLR),and then to the BH mass,using the Full Width at Half Maximum(FWHM) of the broad lines as a surrogate of their dispersion veloc-ity and assuming that the BLR is gravitationally bound to the BH,an assumption con?rmed by detailed studies (Peterson&Wandel1999and2000).In the other AGN the BH masses are determined indirectly assuming that the same relations hold.Wandel(1999)showed that Seyfert galaxies have lower BH to bulge mass ratios than inac-tive galaxies,but the revision of the Magorrian relation leads to conclude?nally that it is not the case(Laor2001, Wandel2002,Gebhardt et al.2000b).
However the status of Narrow Line Seyfert1galax-ies(NLS1s)is not well established in this context.NLS1s constitute about10%of Seyfert nuclei and quasars up to a redshift of0.5(Williams,Pogge,&Mathur2002). Though they are known since a long time(Osterbrock &Pogge1985),their nature is still not well understood. Besides the“narrowness”of their broad lines,these galax-ies share common properties,such as strong FeII permit-ted lines and weak forbidden[OIII]lines,a strong X-ray variability and a big soft X-ray hump(see several reviews in Boller et al.2000).Mathur,Kuraszkiewicz&Czerny (2001)suggested that the BH/bulge mass ratio is smaller in NLS1s,and Wandel(2002)found that M～10?3to 10?4M(Bulge),a smaller value than for broad line AGN (BLS1s).Both papers are based on a very limited sam-ple,and are prone to statistical uncertainties.Moreover, in NLS1s the bulge mass is generally not deduced from the stellar dispersion velocity but from the width of the [OIII]5009line assumed to be proportional to it,follow-ing a suggestion of Nelson and Whittle(1996)for Seyfert 1galaxies(actually Wandel(2002)used direct measure-ments of the bulge luminosity).Wang and Lu(2001)ar-gued that the[OIII]width is not accurately determined in NLS1s,owing to the weakness of the line and to the pres-ence of a blue wing,both e?ects leading to overestimate σ([OIII])and therefore the bulge mass.However Grupe &Mathur(2003)con?rmed the previous result of Mathur et al.(2001)with a complete X-ray selected sample of NLS1s,even when taking into account the presence of the blue wing of the[OIII]line,and she claims that NLS1s occupy distinct regions in the BH/bulge mass relation. Botte et al.(2004)do not con?rm this result,and from a study of the photometric properties of the host galaxies they?nd that the NLS1galaxies seem to share the same BH/bulge mass relation as ordinary Seyfert,and simply occupy the lower ranges of the M?M(Bulge)plane.Bian and Zhao(2003)came to an opposite conclusion,based also on the bulge luminosity(we recall that the relation deduced from the bulge luminosity and the host properties is more dispersed than that deduced from the dispersion velocity),but found that NLS1s do not follow the ordinary relation when using the[OIII]line as an indicator of the dispersion velocity(Bian&Zhao2004).Finally Botte et al.(2004)show that there is a smooth relation between the BH mass vs.the bulge luminosity for di?erent classes of AGN,while there is a jump between the BH mass v.s.the[O III]width.The latter?nding is consistent with what was claimed by Grupe&Mathur(03)and by Bian &Zhao(04).
One sees that the problem of the BH/bulge mass rela-tion in NLS1s is presently highly controversial.It has im-portant cosmological consequences.If BHs in NLS1s are undermassive with respect to their host bulge,it would imply that these galaxies are“young”,in the sense that they are still in the process of building their BH.It would mean that BHs and galaxies do not evolve concomitantly (Mathur2000,and Grupe&Mathur2003).We will show here that there is a strong reason to believe this is true, because NLS1s seem to be accreting at super-Eddington rates and therefore the time scale for the growing of their central black holes could be extremely short.
It is now widely admitted that NLS1s are radiating close to the Eddington luminosity L Edd.This result is simply obtained from the mass-luminosity-FWHM rela-tions mentioned above.A few objects might even have super-Eddington bolometric luminosity,depending on the conversion factor used to transform the optical-UV lumi-nosity into a bolometric one,and on the adopted Hubble constant,but it never exceeds a few L Edd.From this re-sult many people assuming that the e?ciency factor for conversion of mass into energy is constant and of the order of0.1deduce that these objects are also accreting close to their Eddington limit.
But why would it have to be so?Super-Eddington ac-cretion is indeed theoretically allowed.Near the BH,the gas forms an accretion disc,which is supposed to emit the “Big Blue Bump”(BBB).The accretion rate and the BH mass determine the spectral distribution and the?ux of the BBB.It is thus possible to determine the accretion rate when the mass is known.It was performed by Collin et al.(2002,hereafter referred as C02),using the sam-ple of Kaspi et al.(2000)for which the BH masses are deduced from reverberation mapping,and assuming that the optical luminosity is provided by a standard accretion disc(once the luminosity of the underlying galaxy has been subtracted).They found that a fraction of objects is accreting at super-Eddington rates,while their optical lu-minosity stays lower than or of the order of the Eddington luminosity.Actually,when the accretion rate is close to, or larger than the Eddington limit,accretion close to the BH does not proceed through a“thin”,but a“slim”disc whose cooling time is larger than the viscous time,so en-ergy is advected towards the BH before being radiated. The mass-energy conversion e?ciencyηthus decreases as the accretion rate increases,and the luminosity increases only logarithmically with the accretion rate(Abramowicz et al.1988,Wang et al.1999,Fukue2000,Mineshige et al.2000,Wang&Netzer2003,Kawaguchi2003).The emission of such a disc is characterized by a soft X-ray bump as those observed in NLS1s.Kawaguchi(2003), and Kawaguchi,Pierens&Hur′e(2004,hereafter called KPH)have con?rmed that the overall Spectral Energy Distribution(SED)of the two most super-Eddington ac-
Suzy Collin and Toshihiro Kawaguchi:The accretion rate in NLS1s3
cretors are well?tted by the emission of a slim disc. Finally,Wang(2003)noted that super-Eddington accre-tion should lead to a limit relation between the BH mass and the FWHM of the lines,and he found several ob-jects satisfying this relation,indicating that they radiate close to their Eddington luminosity,but accrete above the Eddington limit.
There were only a few NLS1s in the Kaspi et al.sam-ple studied in C02.Moreover the sample is not statistically complete since half of the objects are nearby Seyfert nuclei chosen mainly for their high degree of variability.The re-cent release of several complete samples including a large number of NLS1s,and the renewed interest for these ob-jects since a few years,motivated us to conduct the same study on these new samples.While only standard discs were assumed in C02,here we take into account the devi-ation from the standard disc due to the disc self-gravity, which is particularly important in super-Eddington ob-jects(cf.KPH).We use also the slim disc model to com-pute the bolometric luminosity as a function of the ac-cretion rate.We?nally discuss some observational conse-quences not envisioned in C02.The model can account for the fact that the optical-UV continuum of NLS1s is red-der than that of ordinary Seyferts(Constantin&Shields 2003).The variation of the bolometric luminosity with the accretion rate agrees with the slim disc model.It ex-plains why the FWHMs of the broad lines are larger than 700km/s.
In this paper,we only want to show some general trends and draw qualitative conclusions concerning the accretion rates of NLS1s,using rough theoretical models of accretion discs and applying them to entire samples.
Finally we insist on the fact that all along this paper we accept the commonly admitted statement that the nar-rowness of the lines of NLS1s is not due to an inclination e?ect,i.e.that NLS1s do not constitute a sample of normal Seyfert1nuclei whose broad line region is a rotating disc seen almost face-on.In this case,it is clear that the masses derived from the reverberation mapping formulae would be strongly underestimated,and consequently their lumi-nosity(in terms of Eddington luminosity)overestimated.
In the following section,we recall?rst how BH masses are determined and we present the samples.We discuss the explanation of the empirical relation between the lu-minosity and the size of the BLR.In Section3,we sum-marize the theoretical model.Section4is devoted to a discussion of the results,and in the last section we discuss the alternate possibility that the masses of NLS1s could be underestimated and the accretion rates overestimated.
2.Determination of the BH masses
2.1.The empirical mass-luminosity relation Reverberation mapping studies allowed to determine the size of the BLR in about40objects.It lead to the
dis-Fig.1.Respectively L(5100)(top)and L(5100)/L Edd (bottom)versus the FWHM for all samples.The black (respt.red)triangles indicate the objects with L(5100)
≤0.51044ergs/sec for all samples(respt.the Kaspi et al. sample).The object lying much below the others is NGC
4051.
covery of a correlation between the radius of the re-
gion emitting the Hβline,which we will call R(BLR), and the monochromatic luminosity at5100?A,L(5100)=νLν(5100)(Kaspi et al.2000):
R(BLR)=32.9×L(5100)0.7
44
lt days,(1)
where L(5100)
44
is expressed in1044erg/s.Though there is some uncertainty in the functional form of the rela-tion(https://www.doczj.com/doc/ad8361867.html,or2003,Netzer2003),all recent papers adopt this relation to compute R(BLR)in quasars and Seyfert galaxies,when it has not been determined by reverbera-tion mapping.
It is now well demonstrated that the broad Hβemit-ting region is gravitationally bound to the BH(Peterson &Wandel2000).This gives another relation,M BH= R(BLR)V2/G,where G is the gravitational constant.V is generally taken equal to
√
4Suzy Collin and Toshihiro Kawaguchi:The accretion rate in NLS1s ?ned by FWHM≤2000km/s).Using Eqs.1and2,one
gets a relation between M BH and L(5100)which allows
to determine M BH as a function of the optical luminosity
and the FWHM,without the need to know the size of the
BLR.We stress however that the use of the FWHM as a
surrogate of the dispersion velocity can lead to a system-
atic underestimation of the mass,if the BLR is a relatively
?attened structure dominated by rotation,in which case
the inclination of the system would play an important role
(see Section5).
These relations have important consequences.If one
assumes that L bol～10L(5100),a canonical value for the
quasar continuum(cf.Elvis1994,Laor et al.1997),one
gets from Eqs.1and2:
R Edd=0.35L(5100)0.3
44(FWHM)?2
2000
(3)
=0.28M0.43
7(FWHM)?2.86
2000
lt days,
where we call R Edd the Eddington ratio,i.e.the ratio of
the bolometric upon the Eddington luminosity L Edd= 1.51045M7,and M7the BH mass expressed in107M⊙. It is obvious from this relation that NLS1s have larger
Eddington ratios than BLS1s for a given BH mass.
https://www.doczj.com/doc/ad8361867.html,ments on the luminosity-size relation
There are several possible explanations for this relation. Line emission can be suppressed by dust beyond the radius of sublimation,which corresponds to a given heating?ux
∝L bol/R2(Netzer&Laor1993).But this constraint pro-vides only an outer boundary of the BLR.Nicastro(2000)
proposed that clouds are formed in a wind above the disc, close to the transition region between the gas and the ra-diation pressure dominated zones of the disc.However the size of the BLR depends both on the BH mass and on the luminosity,while the observations give only a luminos-ity dependence.The striking similarity of AGN spectra led also to the idea that the“ionization parameter”(i.e. the radiation pressure to gas pressure ratio or the photon density to gas density ratio,∝L bol/(nR2),n being the electron number density)is constant among all objects. Actually the size-luminosity relation rather implies that the product of the density with the ionization parameter is constant.This is consistent with the so-called“LOC”model.
In1995,Baldwin et al.proposed that the observed spectrum of AGN is simply a consequence of the ability of a photoionized medium to reprocess the underlying con-tinuum“as long as there are enough clouds at the correct radius and with the correct gas density to e?ciently form a given line”.In this“Locally Optimally Emitting Clouds”(or LOC)model,each line is emitted preferentially at an appropriate ionizing?ux L/4πR2corresponding to a given distance from the source1.According to the grid of pho-
Suzy Collin and Toshihiro Kawaguchi:The accretion rate in NLS1s
5 Fig.2.These?gures display˙m as a function of the BH masses for the four samples.The squares give˙m computed according both to the standard disc model(open squares),and to the self-gravitating disc model with a viscosity parameterα=0.01(?lled squares).The crosses give L(5100)/L edd,and the crosses with open circles mark the
NLS1s.The two thick solid lines delineate the position of˙m for the NLS1s.The two horizontal lines correspond to ˙M/˙M
Edd
=1,where˙M Edd=L Edd/(ηc2),in the case of a Schwarzschild BH and of a Kerr BH.The black(respt.red) triangles indicate the objects with L(5100)≤0.51044ergs/sec(respt.for the Kaspi et al.sample).Note that the VVG sample consists only of NLS1s,thus circle symbols are not shown.
given,but for an empty universe,so we made the con-version to q0=0.5.We call this sample Gru03.It is particularly interesting for us as it gives an estimate of the bolometric luminosity of the objects based on the ob-served spectral energy distributions,which we will be able to compare with our models.
We use also two other heterogeneous samples.Wang &Lu(2001)deduced L(5100)from the B-magnitude us-ing the V′e ron-Cetty et al.(2001)sample,which contains 59NLS1s,and they estimated the BH masses using the previous empirical relations.After rejection of a few ob-jects for which the FWHM are controversial,the sample was reduced to54NLS1s.We call it the VVG sample.We also used an heterogeneous sample of soft X-ray selected AGN(Grupe et al.1998,1999),which has the advantage of giving optical indices useful to check our models.We also made the conversion from q0=0to q0=0.5.We call it Gru99.Note that a few objects are also in Gru03.
The samples have not been corrected for the stellar contribution of the host galaxy to the optical luminos-ity.It is certainly important for low luminosity AGN,but not when the optical luminosity is larger than a few1043 ergs/sec.In the following we will distinguish or suppress all these weak objects from the samples,so we can be fairly con?dent that the results will not be contaminated by the host galaxy.
Fig.1displays respectively L(5100)(top)and L(5100)/L Edd(bottom)versus the FWHM for all samples. We note immediately the strong di?erence between these two graphs.While the?rst one shows a very loose cor-
6
Suzy Collin and Toshihiro Kawaguchi:The accretion rate in NLS1s
102
103
104
105
105
106
107
108
109
1010
Fig.3.R sg /R G versus M for all samples,for the self-gravitating disc with α=0.01.The black triangles in-dicate the objects with L(5100)≤0.51044ergs/sec for all samples.
relation,corresponding to the absence of low luminosity objects with large FWHMs and of high luminosity objects with small FWHMs,the second one shows a tight correla-tion with a slope equal to -2,which is expected according to the ?rst line of Eq.3.The black triangles indicate the objects with L(5100)≤0.51044ergs/sec:note that these low luminosity objects share the same relation as the oth-ers.
In an aim of comparison,we have added on these ?g-ures the objects where the BH masses have been deter-mined directly by reverberation mapping (we call these objects the “Kaspi et al.sample”,though half of them were not observed by Kaspi et al.2000).They span the same range of luminosities as the other samples.But ?rst,they show a looser correlation between L(5100)/L Edd and the FWHMs;it is expected as the determination of the mass in the other objects makes use of an exact relation L ?R (BLR),not taking into account its error bars.And second,the relation should be extrapolated to values of the mass and of the Eddington ratio smaller by a factor of 5.It should be kept in mind in the following analysis.Note that the values of the luminosities used in this ?gure correspond to H 0=75km/sec/Mpc,while CO2assumed H 0=50km/sec/Mpc.
3.The accretion disc model
Since more than ?fteen years it is widely admitted that the “infrared bump”at a few microns and the “Big Blue Bump”observed in radio quiet quasars and Seyfert nuclei are both due to thermal emission,respectively by hot dust
heated by the UV-X continuum,and by the accretion disc (Sanders et al.1989).In this picture,the observed “dip”at ～5000?A in the log(νF ν)versus log νcurve corresponds to the junction between these two processes,the hot dust close to the sublimation temperature (1700K)being un-able to radiate appreciably below 1μm.In particular the idea of an underlying non-thermal power law continuum which was invoked in the past and used to model the in-frared to UV emission of AGN has been completely left over.So the emission at 5000?A should be due entirely to the accretion disc ,unless another medium can give rise to a smooth featureless optical continuum.The problem was discussed in C02,and they showed that it would require the existence of a very dense,optically thick and relatively cold medium.It is di?cult to ?nd for such a medium an-other location than an optically thick accretion disc.
For a “standard”thin Keplerian disc where gravita-tional energy is released locally through turbulent viscos-ity,the e?ective temperature T e?at a distance R from a BH of mass M is:
σT 4
e?=
3GM ˙M c 2
Rout
Rin
RdR
Suzy Collin and Toshihiro Kawaguchi:The accretion rate in NLS1s7 the photon trapping radius to the vicinity of the central
BH(Shimura&Manmoto2003;Kawaguchi2003)is neces-
sary in order to discuss the broad-band spectra of NLS1s.
We use the slim disc model for a Schwarzshild BH com-
puted as in Kawaguchi(2003),which is based on the code
developed by Matsumoto et al.(1984).The e?ect of elec-
tron scattering(both in opacity and Comptonization)and
relativistic correction are included.We take the viscosity
parameterαequal to0.1.Note that the slim disc is used
here only to compute the bolometric luminosity.
Even if the accretion rate is very high(in Eddington
value)the optical luminosity is still emitted at a large ra-
dius where the accretion?ow is not in?uenced by advec-
tion and photon trapping,except in the case of very high
accretion rates(˙M≥3103L Edd/c2,cf.KPH),and the
standard disc model is valid.The only deviation to the lo-
cal blackbody in the optical region is due to electron scat-
tering(as modi?ed blackbody,see Czerny&Elvis1987),
which distorts the spectrum for super-Eddington accretion
rates.It is negligible as far as viscosity is small(α≤0.1)
and the BH mass is small(M≤107M⊙),so the distortion
is not very important for NLS1s(cf.KPH),and we will
neglect it in this paper.
However an important fact should not be forgotten,
which acts also for modest accretion rates but is very im-
portant for super-Eddington accretion rates.
At about the distance of the optical emitting region,
the disc becomes self-gravitating,i.e.the vertical compo-
nent of the BH gravity becomes smaller than the disc’s
own gravity.This occurs beyond a critical radius R sg cor-
responding to a density:
?2K
ρsg=
8Suzy Collin and Toshihiro Kawaguchi:The accretion rate in NLS1s
this case one?nds thatλ(105R g)～20M1/4
7˙m?1/4μm,
which insures that the optical emission is entirely pro-duced inside105R g.On the contrary,if the disk extends only up to103R g or104R g,the computed optical emission
would be smaller than for R out=105R g,and the accretion rate would therefore be larger.
As an accretion disc with a super-Eddington accretion
rate behaves like a standard disc outside the photon trap-ping radius(KPH),we compute R sg with the same analyt-
ical approximation as KPH,which gives expressions simi-lar to the previous detailed computations of Hur′e(1998): R sg= R3sg,a+R3sg,b+R3sg,c 1/3(7) where R sg,a,R sg,b,and R sg,c are the self-gravitation ra-
dius in respectively the inner region dominated by radia-tion pressure and Thomson opacity,the intermediate re-gion,dominated by gas pressure and Thomson opacity, the outer region dominated by gas pressure and atomic opacity:
R sg,a=500 αL Edd/c2 4/9R G(8) R sg,b=11400 αL Edd/c2 ?8/27R G R sg,c=13400 αL Edd/c2 ?22/45R G.
These expressions depend on the viscosity parameterα. We will useα=0.3,α=0.1,andα=0.01.A smaller value ofαhas a more profound in?uence on the disc struc-ture,as it corresponds to a denser standard disc,and therefore a smaller value of R sg.
Let us now discuss the consequences of these relations
in an approximate way.As we shall see later,none of the free parameters have a strong in?uence on the com-puted accretion rate,the main quantity that we want
to determine.We have seen that for a standard disc,
L(5100)∝(M˙M)2/https://www.doczj.com/doc/ad8361867.html,ing this relation,and Eqs.1and 2,we get:
˙m∝FWHM?4.28M0.14,(9) where˙m is the accretion rate expressed in Eddington units,˙m=˙M
Suzy Collin and Toshihiro Kawaguchi:The accretion rate in NLS1s
9
-0,5
0,5
1
1,5
2
2,5
3
103
104
Gru99
https://www.doczj.com/doc/ad8361867.html,parison between the observed and computed optical spectral index αopt ,for the Gru99sample,exclud-ing the objects with L(5100)≤0.51044erg/s.The black ?lled circles are the observed values,the open symbols are computed with the self-gravitating correction,for αequal respectively to 0.01(blue circles)and 0.1(red squares).We recall that αopt =0.3for a standard disc.
all computations,cos(i )is set equal to 0.75.The objects with L(5100)≤0.51044ergs/sec are indicated on the ?g-ures.There are only two such objects (actually lying close to the limit)in Bor03.The Gru03sample contains many low luminosity objects,but a large number of NLS1s are above the luminosity limit.
We see that the self-gravitation correction can decrease ˙m by about a factor three for large values of ˙m ,but has no in?uence on small ˙m .For larger values of αand of γ,the di?erence between the standard and the self-gravitating disc would be smaller.So we can consider that the two models here correspond to a kind
of “error bar”on ˙m ,for given BH mass and L(5100).Figs.2shows also the “observed”ratio L(5100)/L Edd .We have noted the NLS1s,and the thick dotted lines delineate the position of ˙m for NLS1s.NLS1s always have BH masses smaller than 108M ⊙,and they are located in the higher range of L(5100)/L edd and ˙m .It is interesting to note that the four samples do not di?er except for the range of masses and luminosities,though they have been selected quite di?er-ently.
Again we added for comparison to these ?gures the results for the Kaspi et al.sample,computed using only the standard disc emission (we recall that the results di?er from CO2because we use here H 0=75instead of 50).As expected,the extrapolation by a factor 5in mass range of the empirical relationship translates in an extrapolation of
˙m by about a factor 30,as ˙m ∝˙M/M BH ∝L 3/25100×M ?2BH .
Fig.6.Accretion rates in M ⊙/yr for the four samples as
a function of the BH masses,excluding the objects with L(5100)≤0.51044erg/s,and computed according to the self-gravitating disc model with a viscosity parameter α=0.01.NLS1s are indicated as red dots.
Several other results appear on these ?gures.First ˙m increases as the BH mass decreases .On the contrary,the ratio L(5100)/L Edd is always smaller than 0.3,and seems about constant for the NLS1s.When ap-plying a standard correction L bol ～10×L(5100),one concludes that L bol saturates at about the Eddington lu-minosity,whatever the BH mass .This excludes the ex-istence of the large super-Eddington ratios proposed by Begelman (2002)due to the photon bubble instability.Thus,according to Eq.3,there should be a lower limit
to the FWHMs of the order of 1000M 0.15
7km/s unless the empirical relations do not apply to these objects.And indeed FWHMs of the order of 100-500km/s which would imply Eddington ratios larger than 10have never been ob-served in Seyfert 1nuclei.
Second,the two horizontal lines correspond to ˙M/
˙M Edd =1,where ˙M Edd =L Edd /(ηc 2),in the case of a Schwarschild BH (η=0.057)and of an extremely rotating Kerr BH (η=0.30).We see that the accretion rates of NLS1s are always larger than the Eddington rate in the case of Kerr BHs,and mostly larger in the case of Schwarzschild BHs .
There are several causes of uncertainties in the results (cf.Krolik 2001and C02),which might introduce errors on the BH masses as large as one order of magnitude,because one should not forget that even the masses de-termined directly with reverberation mapping are known with an uncertainty of a factor 3.It seems however im-plausible that all the uncertainties would systematically act towards an underestimation of the mass and an over-
10
Suzy Collin and Toshihiro Kawaguchi:The accretion rate in NLS1s 0,01
0,1
1
10
102
10-2
10-1
100
101
102
103
Gru03
Fig.7.The Eddington ratio R edd as a function of ˙m for the Gru03sample,computed with the standard disc (open squares)and the self-gravitating disc,α=0.01(?lled squares).The objects with L(5100)≤0.51044ergs/sec have been suppressed.The two curves correspond to the slim disc model,α=0.1,and respectively a Schwarzshild and a kerr BH.
estimation of the luminosity,avoiding the conclusion of super-Eddington accretion rates.Only the uncertainty on the correcting factor of the FWHM due to the geome-try and kinematics of the BLR could lead to a systematic underestimation of the mass,if the BLR is a rotating ?at structure.It can be large when the objects are seen almost face-on.We shall discuss this point in the last section.Fig.3displays R sg /R G versus M for all samples,for the self gravitating disc with α=0.01.We note that it is always quite small (in particular smaller than the BLR,which has typical values 103for high BH masses and 105for NLS1s),justifying our previous claim that the BLR is always located in,or above,the unstable part of the disc.As expected R sg /R G decreases with the BH mass,except at the high mass limit,and there is a strong correlation between the two parameters.
Although the choice of parameters for the self-gravitating disc does not in?uence strongly ˙m ,it has an e?ect on the optical spectral index.As an illustration,Fig.4shows the computed optical spectral index αopt de?ned as F ν∝ν?αopt between 4400and 7000?A (rest frame),for the Bor03sample.The computation is performed with the self-gravitating correction,for a viscosity parameter
αequal to 0.01,0.1,and 0.3.A systematic correction E (B ?V )=0.05for the galactic absorption has been ap-plied (certainly an underestimation).For α=0.01,the continuum is red except for very broad line objects.The trend that broader objects have bluer optical spectra is consistent with the observational results of Constantin &Shields (2003).The continuum is globally bluer for smaller values of α(0.1and 0.3).We also see that αopt almost never reaches the value of the standard disc (-0.33).A de-tailed comparison with the observed values is postponed to the next paper.
Fig.5shows a comparison between the observed and computed spectral indexes for the Gru99sample,exclud-ing the objects with L(5100)≤0.51044erg/s.According to Grupe et al.(1999),the observed values of αopt are given with an uncertainty of ±0.4.With α=0.1,many of the computed indices are close to the value of the stan-dard disc,while the objects of the samples are particularly red,with an average index of 0.8.The agreement is much better for the smallest viscosity parameter α=0.01.The very red spectra observed in a fraction of objects might be due to intrinsic reddening not taken into account in the computed values.If it is the case,it would imply that the observed L(5100)is underestimated in these objects,but again it is not important for the determination of ˙m .Note that in this sample,NLS1s do not seem to have redder continua than BLR1s.
It is therefore impossible from this comparison to de-cide which are the best values of αand γto choose for the disc.Our model is clearly oversimpli?ed,and would require a more sophisticated parametrization.The only conclusion which can be drawn is that a non-standard disc with an additional release of energy in its external region gives a better ?t to the average optical continuum of AGN than a standard disc.However,this problem does not question the existence of super-Eddington accretion rates for NLS1s.
Finally Fig.6displays the accretion rates in M ⊙/yr for the four samples,excluding the objects with L(5100)≤0.51044erg/s,and computed according to the self-gravitating disc model with a viscosity parameter α=0.01.Note that the imposed limit on L(5100)creates the
sharp limitation on the left side,as ˙M
is proportional to M ?2/3(for a ?xed L opt ).The limitation on the right side is due to a limitation of ˙m at about 0.03(perhaps due to the fact that the accretion disc changes into an ADAF be-low this value).NLS1s are indicated as red dots.Despite the large values of ˙m of NLS1s,we see that the maximum accretion rate is of the order of one M ⊙/yr whatever the BH mass .This is a strong indication of an exterior regu-lation of the accretion ,rather than the self-regulation of the disc.Note that it is a modest value when compared with the rate of star formation in a starburst nucleus.
Suzy Collin and Toshihiro Kawaguchi:The accretion rate in NLS1s
11
Fig.8.Cumulative number of objects(normalized to unity)on which an underestimation of the mass by a fac-tor smaller than M real/M obs is made,in the conditions explained in the text.
https://www.doczj.com/doc/ad8361867.html,parison with the slim disc model
It is interesting to compare the observed SED of super-Eddington objects with the slim disc model.As we mentioned in the introduction,this was done in de-tail for the two highest˙m objects(Kawaguchi2003; KPH;Kawaguchi,Matsumoto,Leighly in preparation;see Kawaguchi2004).and it will be performed for the objects of the samples in a future paper.Here we simply com-pute the bolometric luminosity,and we compare it with the observed values.
Only the Gru03sample provides bolometric luminosi-ties based on the observed SEDs.Fig.7shows the ob-served ratio R Edd versus˙m for this sample.The low lu-minosity nuclei(L(5100)≤0.51044ergs/sec)have been suppressed.Also shown is the theoretical curves obtained for the slim disc model with a Schwarzschild and a Kerr BH.These curves depend very little on the BH mass and on the viscosity parameter.In spite of the large dispersion of the“observations”,it is clear that a majority of points lie above the Schwarzschild curve,meaning that the e?-ciency of the Schwarzschild BH is insu?cient,i.e.a Kerr BH with an e?ciency of about0.15would better?t the ob-servations unless there is a systematic underestimation of the BH masses.On the other hand,the shape of the curve agrees well with the observed points,in particular in the “saturation”of R Edd above˙m=10.Three objects reach an Eddington ratio of the order of10,for50≤˙m≤1000.
5.In?uence of the inclination on the masses and
accretion rates
In all mass determinations,the FWHM is used instead of the dispersion velocity.It makes the implicit assumption that the velocities are distributed at random in the BLR.However,if the BLR is a?at structure dominated by ro-tation,the FWHM is proportional to sin(i)V Kep,where i is the angle between the normale and the line of sight(the inclination).It is clear that a small inclination can lead to a large underestimation of V Kep and therefore of the mass.
However the BLR cannot be a geometrically thin disc with an exactly Keplerian velocity.Unfortunately its dy-namics and its structure are still not well determined from detailed reverberation mappings,but we know that it should be at least a“thick disc”,with an aspect ratio larger than,say,H/R～0.3(H being the disc thickness at the radius R),since it needs to have a large coverage factor of the central source.Such a disc must be sustained vertically by a turbulent pressure corresponding to a tur-bulent velocity of the order of V Kep H/R.The FWHM is then proportional to V Kep
dG
=
[(H/R)2+sin(i)2]2
12Suzy Collin and Toshihiro Kawaguchi:The accretion rate in NLS1s
Eddington limit,however at a smaller rate.On the other hand,it is quite possible that the few extremely high ac-cretors are actually“face-on”objects,and that their mass is indeed underestimated by about one order of magni-tude.
6.Conclusion
We used the BH masses deduced from the size-luminosity relationship to compute their accretion rate in four sam-ples of AGN,assuming that the optical luminosity is pro-vided by the accretion disc.Thus the empirical relation must be extrapolated in a range of masses almost one or-der of magnitude smaller than the Kaspi et al.sample. We used a simpli?ed disc model,with a parametrization of the energy release in the self-gravitating region to get the accretion rate,and the slim disc model in the inner re-gions in order to get the bolometric luminosity.In spite of the crudeness of the treatment,this study leads to several fairly certain conclusions.
–NLS1s are always accreting at Eddington or super-Eddington rates.˙m can reach1000,corresponding to an accretion rate equal to60˙M Edd(for Schwarzschild BH)and to300˙M Edd(for Kerr BH).
–Their observed bolometric luminosities“saturate”at ～10Eddington luminosities,as predicted by slim disc models.It explains why there is a lower limit to the observed FWHM.
–The observed value of the bolometric luminosities are in better agreement with a Kerr than with a Schwarzschild BH.
–The computed optical spectral indexes agree with the observed trend of redder spectra for NLS1s than for BLS1s.
–And?nally the accretion rates have an upper limit of about one M⊙/yr,whatever the BH mass.In partic-ular,all NLS1s have an accretion rate of this order.
This is a strong indication for a mass limited supply, implying an exterior regulation of the accretion.
With these results we are in a position to say now that NLS1s should have a strong in?uence on the growth of BHs.This is in agreement with the claim by Mathur et al. 2001,and Grupe&Mathur2004.Since NLS1s constitute about10%of normal Seyfert which themselves are about 2%of inactive galaxies,one deduces that all galaxies spend 0.2%of their lifetime in the NLS1phase,i.e.2107years. During this time the mass of the BH increases by one order of magnitude(Kawaguchi et al.2004).This could account both for the observed large dispersion in the BH/bulge mass relation of NLS1s,and for the existence of undermas-sive BH/bulge ratios during a large fraction of the NLS1 phase.The increase of the bulge mass could have taken place during merger or interaction events.BHs would then grow during intense phases of activity after a time delay, necessary for accumulating matter in the circumnuclear region and for triggering a starburst.In this scenario,the overabundance of iron could be easily explained by the rapid formation of massive stars and supernovae explo-sions in the outer parts of the accretion disc where the accretion rate is high(Collin&Zahn2000,Levin2003, Levin&Belobodorov2003).The scenario would also ac-count naturally for the presence of out?ows giving rise to the blue wing of the[OIII]line,as super-Eddington accre-tion is expected to generate out?ows by strong radiation ?elds.
Though we have tried to determine a lower limit of the accretion rate,two e?ects can intervene to still reduce it. They were both discussed in C02.
1-the possibility that the accretion rate decreases with the radius between the optically emitting region and the BH, owing to the creation of a strong out?ow due to the radi-ation pressure.The accretion rate close to the BH would then be just Eddington.In this case,the out?ow could well be the origin of the[OIII]wing,and could lead to the escape of a part of the Narrow Line Region,explain-ing the weakness of the[OIII]line.However,one should realize that in this case the rate of out?ow would have to represent90or even99%of the accretion rate,in the highest accretors.This seems unrealistic.
2-The optical luminosity is not provided by the accretion disc.Recently King&Pounds(2003)suggested that BHs accreting at super Eddington rate produce winds which are Thomson thick and can emit a black body spectrum providing the Blue Bump of AGN.Pounds et al.(2003) indeed report that they have found the signature of such an optically thick wind in the X-ray spectrum of the NLS1 PG1211+143.If the existence of such a wind is con?rmed in other NLS1s,then it is clear that the present analysis would have to be reconsidered.However let us recall that Collin et al.(2002)have shown that very strong conditions must be met in such a wind to give rise to the optical-UV featureless continuum:it must have both a large density (1014cm?3),and a Thomson thickness at least of unity. Besides,to get the observed luminosity,it should be lo-cated far from the center and it should have a large spatial extension.It is thus not obvious that the wind observed by Pounds et al.(2003)satis?es these requirements.It is more likely that its emission is limited only to the EUV radiation,and that the optical emission is still due to the accretion disc.
We have assumed all along the paper that the BH masses of NLS1s are correctly estimated by the empirical reverberation relations,even when these relations had to be extrapolated by almost one order of magnitude.On the other hand,we have accepted the usual assumption that the FWHM is a good measure of the velocity in the BLR, implicitly assuming that the velocities are distributed at random.If on the contrary the BLR is a?at structure dominated by rotation,the BH masses of a fraction of ob-jects could be underestimated by factors up to one order of magnitude and the accretion rates(in terms of Eddington)
Suzy Collin and Toshihiro Kawaguchi:The accretion rate in NLS1s13
by two order of magnitudes when they are seen nearly face-on.However,since this fraction should be small,we think that the scenario described in this paper is qualitatively correct.
Acknowledgements.We are grateful to Amri Wandel for useful comments which have contributed to improve substantially the paper.
References
Abramowicz,M.A.,Czerny,B.,Lasota,J.P.,&Szuszkiewicz,
E.1988,ApJ,332,646
Antonucci,R.R.J.,Miller,J.S.1985,ApJ197,621
Baldwin,J.,Ferland,G.,Korista,K.,&Verner,D.1995,ApJ, 455,L119
Begelman M.C.1978,MNRAS,184,53
Begelman,M.C.2002,ApJ,568,L97
Bian,W.&Zhao,Y.2003,Chin.J.Astron.Astrophys.2,119 Bian,W.&Zhao,Y.2004,MNRAS,347,607
Boller,T.2000,New Astronomy Review,44
Boroson,T.A.2003,ApJ,585,647
Botte,V.,Ciroi,S.,Rafanelli,P.,Di Mille, F.2004, astro-ph/0402627
Collin-Sou?rin,S.&Dumont,A.M.1989,A&A,213,29 Collin,S.&Zahn,J.1999,A&A,344,433
Collin,S.&Hur′e,J.1999,A&A,341,385
Collin,S.2001,Advanced Lectures on the Starburst-AGN, 167
Collin,S.&Hur′e,J.-M.2001,A&A,372,50
Collin,S.,Boisson,C.,Mouchet,M.,Dumont,A.-M.,Coup′e, S.,Porquet,D.,&Rokaki,E.2002,A&A,388,771(C02) Constantin,A.&Shields,J.C.2003,PASP,115,592 Czerny,B.&Elvis,M.1987,ApJ,321,305
Elvis,M.,et al.1994,ApJS,95,1
Ferland,G.J.&Rees,M.J.1988,ApJ,332,141 Ferrarese,L.&Merritt,D.2000,ApJ,539,L9
Ferrarese,L.,Pogge,R.W.,Peterson, B.M.,Merritt, D., Wandel,A.,&Joseph,C.L.2001,ApJ,555,L79 Frank,J.,King,A.,&Raine,D.J.2002,Accretion Power in Astrophysics:Third Edition,by Juhan Frank,Andrew King,and Derek J.Raine.Cambridge University Press, 2002,398
Fukue,J.2000,PASJ,52,829
Gebhardt,K.,et al.2000a,ApJ,539,L13
Gebhardt,K.,et al.2000b,ApJ,543,L5
Goldreich,P.&Lynden-Bell,D.1965,MNRAS,130,97 Grupe,D.,Beuermann,K.,Thomas,H.-C.,Mannheim,K.,& Fink,H.H.1998,A&A,330,25
Grupe,D.,Beuermann,K.,Mannheim,K.,&Thomas,H.-C.
1999,A&A,350,805
Grupe,D.,Mathur,S.2003,astro-ph/0312390
Grupe,D.,Wills,B.J.,Leighly,K.M.,&Meusinger,H.2004, AJ,127,156
Haehnelt,M.G.,Natarajan,P.,&Rees,M.J.1998,MNRAS, 300,817
Haehnelt,M.G.&Kau?mann,G.2000,MNRAS,318,L35 Hatziminaoglou,E.,Mathez,G.,Solanes,J.,Manrique,A.,& Salvador-Sol′e,E.2003,MNRAS,343,692
Hur′e,J.1998,A&A,337,625
Kaspi,S.,Smith,P.S.,Netzer,H.,Maoz,D.,Jannuzi,B.T., &Giveon,U.2000,ApJ,533,631
Kawaguchi,T.2003,ApJ,593,69Kawaguchi,T.,Pierens,A.,&Hur′e,J.-M.2004,A&A,415,47 (KPH)
Kawaguchi,T.2004,in Stellar-Mass,Intermediate-Masss, and Supermassive Black Holes,eds.K.Makishima&S.
Mineshige,to appear in Progress of Theoretical Physics, Supplement
Kawaguchi,T.,Aoki,K.,Ohta,K.,Collin,S.2004,A&A,420, L23
King,A.2003,ApJ.596,L27
King,A.R.&Pounds,K.A.2003,MNRAS,345,657 Korista,K.,Baldwin,J.,Ferland,G.,&Verner,D.1997,ApJS, 108,401
Koratkar,A.&Blaes,O.1999,PASP,111,1
Krolik,J.H.&Begelman,M.C.1988,ApJ,329,702
Laor,A.,Fiore,F.,Wilkes,B.,Elvis,M.,McDowell,J.1997, ApJ,477,93
Laor,A.2001,ApJ,553,677
Laor,A.2003,ApJ,590,86
Levin,Y.&Beloborodov,A.M.2003,ApJ,590,L33 Lodato,G.&Bertin,G.2003,ASP Conf.Ser.290:Active Galactic Nuclei:From Central Engine to Host Galaxy,223 Magorrian,J.,et al.1998,AJ,115,2285
Marconi,A.,Risaliti,G.,Gilli,R.,Hunt,L.K.,Maiolino,R., Salvati,M.2004,MNRAS,in press,astro-ph/0311619 Mathur,S.,Kuraszkiewicz,J.,&Czerny, B.2001,New Astronomy,6,321
Mathur,S.2000,New Astronomy Review,44,469 Matsumoto,R.,Kato,S.,Fukue,J.&Okazaki,A.T.1984, PASJ,36,761
Menou,K.,Haiman,Z.,&Narayanan,V.K.2001,ApJ,558, 535
Mineshige,S.,Kawaguchi,T.,Takeuchi,M.,&Hayashida,K.
2000,PASJ,52,499
Nelson,C.H.&Whittle,M.1996,ApJ,465,96
Netzer,H.&Laor,A.1993,ApJ,404,L51
Netzer,H.2003,ApJ,583,L5
Nicastro,F.2000,ApJ,530,L65
Osterbrock,D.E.&Pogge,R.W.1985,ApJ,297,166 Peterson,B.M.&Wandel,A.1999,ApJ,521,L95 Peterson,B.M.&Wandel,A.2000,ApJ,540,L13 Pounds,K.A.,Reeves,J.N.,King,A.R.,Page,K.L.,O’Brien, P.T.,&Turner,M.J.L.2003,MNRAS,345,705 Sanders,D.B.,Phinney,E.S.,Neugebauer,G.,Soifer,B.T., &Matthews,K.1989,ApJ,347,29
Shimura,T.&Manmoto,T.2003,MNRAS,338,1013
Silk,J.&Rees,M.J.1998,A&A,331,L1
Soria,R.&Puchnarewicz,E.M.2002,MNRAS,329,456 Tremaine,S.,et al.2002,ApJ,574,740
Umemura,M.2001,ApJ,560,L29
V′e ron-Cetty,M.-P.,V′e ron,P.,&Gon?c alves,A.C.2001,A&A, 372,730
Wandel,A.1999,ApJ,527,649
Wandel,A.1999,ApJ,519,L39
Wandel,A.,Peterson,B.M.,&Malkan,M.A.1999,ApJ,526, 579
Wandel,A.2002,ApJ,565,762
Wang,J.,Szuszkiewicz,E.,Lu,F.,&Zhou,Y.1999,ApJ,522, 839
Wang,T.&Lu,Y.2001,A&A,377,52
Wang,J.-M.&Netzer,H.2003,A&A,398,927
Wang,J.2003,AJ,125,2859
Williams,R.J.,Pogge,R.W.,&Mathur,S.2002,AJ,124, 3042
JOIN IN 学生用书1 Word List Starter Unit 1.Good afternoon 下午好 2.Good evening 晚上好 3.Good morning 早上好 4.Good night 晚安 5.Stand 站立 Unit 1 6.count [kaunt] （依次）点数 7.javascript:;eight [eit] 八 8.eleven [i'levn] 十一 9.four [f?:] 四 10.five [faiv] 五 11.flag [fl?g] 旗 12.guess [ges] 猜 13.jump [d??mp] 跳 14.nine [nain] 九 15.number ['n?mb?] 数字 16.one [w?n] 一 17.seven ['sevn] 七 18.six [siks] 六 19.ten [ten] 十 20.three [θri:] 三 21.twelve [twelv] 十二 22.two [tu:] 二 23.your [ju?] 你的 24.zero ['zi?r?u] 零、你们的 Unit 2 25.black [bl?k] 黑色26.blue [blu:] 蓝色 27.car [kɑ:] 小汽车 28.colour ['k?l?] 颜色 29.door [d?:] 门 30.favourite [feiv?rit]javascript:; 特别喜爱的 31.green [gri:n] 绿色 32.jeep [d?i:p] 吉普车 33.orange ['?:rind?] 橙黄色 34.pin k [pi?k] 粉红色 35.please [pli:z] 请 36.purple ['p?:pl] 紫色 37.red [red] 红色 38.white [wait] 白色 39.yellow ['jel?u] 黄色 Unit 3 40.blackboard ['bl?kb?:d] 黑板 41.book [buk] 书 42.chair [t???] 椅子 43.desk [desk] 桌子 44.pen [pen] 钢笔 45.pencil ['pensl] 铅笔 46.pencil case [keis] 笔盒 47.ruler ['ru:l?] 尺、直尺 48.schoolbag [sku:l] 书包 49.tree [tri:] 树 50.window ['wind?u] 窗、窗口 Unit 4 51.brown [braun] 棕色 52.cat [k?t] 猫
常用整流二极管 型号VRM/Io IFSM/ VF /Ir 封装用途说明1A5 600V/1.0A 25A/1.1V/5uA[T25] D2.6X3.2d0.65 1A6 800V/1.0A 25A/1.1V/5uA[T25] D2.6X3.2d0.65 6A8 800V/6.0A 400A/1.1V/10uA[T60] D9.1X9.1d1.3 1N4002 100V/1.0A 30A/1.1V/5uA[T75] D2.7X5.2d0.9 1N4004 400V/1.0A 30A/1.1V/5uA[T75] D2.7X5.2d0.9 1N4006 800V/1.0A 30A/1.1V/5uA[T75] D2.7X5.2d0.9 1N4007 1000V/1.0A 30A/1.1V/5uA[T75] D2.7X5.2d0.9 1N5398 800V/1.5A 50A/1.4V/5uA[T70] D3.6X7.6d0.9 1N5399 1000V/1.5A 50A/1.4V/5uA[T70] D3.6X7.6d0.9 1N5402 200V/3.0A 200A/1.1V/5uA[T105] D5.6X9.5d1.3 1N5406 600V/3.0A 200A/1.1V/5uA[T105] D5.6X9.5d1.3 1N5407 800V/3.0A 200A/1.1V/5uA[T105] D5.6X9.5d1.3 1N5408 1000V/3.0A 200A/1.1V/5uA[T105] D5.6X9.5d1.3 RL153 200V/1.5A 60A/1.1V/5uA[T75] D3.6X7.6d0.9 RL155 600V/1.5A 60A/1.1V/5uA[T75] D3.6X7.6d0.9 RL156 800V/1.5A 60A/1.1V/5uA[T75] D3.6X7.6d0.9 RL203 200V/2.0A 70A/1.1V/5uA[T75] D3.6X7.6d0.9 RL205 600V/2.0A 70A/1.1V/5uA[T75] D3.6X7.6d0.9 RL206 800V/2.0A 70A/1.1V/5uA[T75] D3.6X7.6d0.9 RL207 1000V/2.0A 70A/1.1V/5uA[T75] D3.6X7.6d0.9 RM11C 1000V/1.2A 100A/0.92V/10uA D4.0X7.2d0.78 MR750 50V/6.0A 400A/1.25V/25uA D8.7x6.3d1.35 MR751 100V/6.0A 400A/1.25V/25uA D8.7x6.3d1.35 MR752 200V/6.0A 400A/1.25V/25uA D8.7x6.3d1.35 MR754 400V/6.0A 400A/1.25V/25uA D8.7x6.3d1.35 MR756 600V/6.0A 400A/1.25V/25uA D8.7x6.3d1.35 MR760 1000V/6.0A 400A/1.25V/25uA D8.7x6.3d1.35 常用整流二极管(全桥） 型号VRM/Io IFSM/ VF /Ir 封装用途说明RBV-406 600V/*4A 80A/1.10V/10uA 25X15X3.6 RBV-606 600V/*6A 150A/1.05V/10uA 30X20X3.6 RBV-1306 600V/*13A 80A/1.20V/10uA 30X20X3.6 RBV-1506 600V/*15A 200A/1.05V/50uA 30X20X3.6 RBV-2506 600V/*25A 350A/1.05V/50uA 30X20X3.6 常用肖特基整流二极管SBD 型号VRM/Io IFSM/ VF Trr1/Trr2 封装用途说明EK06 60V/0.7A 10A/0.62V 100nS D2.7X5.0d0.6 SK/高速 EK14 40V/1.5A 40A/0.55V 200nS D4.0X7.2d0.78 SK/低速 D3S6M 60V/3.0A 80A/0.58V 130p SB340 40V/3.0A 80A/0.74V 180p SB360 60V/3.0A 80A/0.74V 180p SR260 60V/2.0A 50A/0.70V 170p MBR1645 45V/16A 150A/0.65V <10nS TO220 超高速
常用二极管参数 2008-10-22 11:48 05Z6.2Y 硅稳压二极管 Vz=6~6.35V, Pzm=500mW, 05Z7.5Y 硅稳压二极管 Vz=7.34~7.70V, Pzm=500mW, 05Z13X 硅稳压二极管 Vz=12.4~13.1V, Pzm=500mW, 05Z15Y 硅稳压二极管 Vz=14.4~15.15V, Pzm=500mW, 05Z18Y 硅稳压二极管 Vz=17.55~18.45V, Pzm=500mW, 1N4001 硅整流二极管 50V, 1A,(Ir=5uA, Vf=1V, Ifs=50A) 1N4002 硅整流二极管 100V, 1A, 1N4003 硅整流二极管 200V, 1A, 1N4004 硅整流二极管 400V, 1A, 1N4005 硅整流二极管 600V, 1A, 1N4006 硅整流二极管 800V, 1A, 1N4007 硅整流二极管 1000V, 1A, 1N4148 二极管 75V, 4PF, Ir=25nA, Vf=1V, 1N5391 硅整流二极管 50V, 1.5A,(Ir=10uA, Vf=1.4V, Ifs=50A) 1N5392 硅整流二极管 100V, 1.5A, 1N5393 硅整流二极管 200V, 1.5A, 1N5394 硅整流二极管 300V, 1.5A, 1N5395 硅整流二极管 400V, 1.5A, 1N5396 硅整流二极管 500V, 1.5A, 1N5397 硅整流二极管 600V, 1.5A, 1N5398 硅整流二极管 800V, 1.5A, 1N5399 硅整流二极管 1000V, 1.5A, 1N5400 硅整流二极管 50V, 3A,(Ir=5uA, Vf=1V, Ifs=150A) 1N5401 硅整流二极管 100V, 3A, 1N5402 硅整流二极管 200V, 3A, 1N5403 硅整流二极管 300V, 3A, 1N5404 硅整流二极管 400V, 3A, 1N5405 硅整流二极管 500V, 3A, 1N5406 硅整流二极管 600V, 3A, 1N5407 硅整流二极管 800V, 3A, 1N5408 硅整流二极管 1000V, 3A, 1S1553 硅开关二极管 70V, 100mA, 300mW, 3.5PF, 300ma, 1S1554 硅开关二极管 55V, 100mA, 300mW, 3.5PF, 300ma, 1S1555 硅开关二极管 35V, 100mA, 300mW, 3.5PF, 300ma, 1S2076 硅开关二极管 35V, 150mA, 250mW, 8nS, 3PF, 450ma, Ir≤1uA, Vf≤0.8V,≤1.8PF, 1S2076A 硅开关二极管 70V, 150mA, 250mW, 8nS, 3PF, 450ma, 60V, Ir≤1uA, Vf≤0.8V,≤1.8PF, 1S2471 硅开关二极管80V, Ir≤0.5uA, Vf≤1.2V,≤2PF, 1S2471B 硅开关二极管 90V, 150mA, 250mW, 3nS, 3PF, 450ma, 1S2471V 硅开关二极管 90V, 130mA, 300mW, 4nS, 2PF, 400ma, 1S2472 硅开关二极管50V, Ir≤0.5uA, Vf≤1.2V,≤2PF, 1S2473 硅开关二极管35V, Ir≤0.5uA, Vf≤1.2V,≤3PF,
Join In剑桥小学英语(改编版)入门阶段Unit 1Hello,hello第1单元嗨,嗨 and mime. 1 听,模仿 Stand up Say 'hello' Slap hands Sit down 站起来说"嗨" 拍手坐下来 Good. Let's do up Say 'hello' Slap hands Sit down 好. 我们来再做一遍.站起来说"嗨"拍手坐下来 the pictures. 2 再听一遍给图画编号. up "hello" hands down 1 站起来 2 说"嗨" 3 拍手 4 坐下来说 3. A ,what's yourname 3 一首歌嗨,你叫什么名字 Hello. , what's yourname Hello. Hello. 嗨. 嗨. 嗨, 你叫什么名字嗨,嗨. Hello, what's yourname I'm Toby. I'm Toby. Hello,hello,hello.嗨, 你叫什么名字我叫托比. 我叫托比 . 嗨,嗨,嗨. I'm Toby. I'm Toby. Hello,hello, let's go! 我是托比. 我是托比. 嗨,嗨, 我们一起! Hello. , what's yourname I'm 'm Toby. 嗨.嗨.嗨, 你叫什么名字我叫托比.我叫托比. Hello,hello,hello. I'm 'm Toby. Hello,hello,let's go! 嗨,嗨,嗨.我是托比. 我是托比. 嗨,嗨,我们一起! 4 Listen and stick 4 听和指 What's your name I'm Bob. 你叫什么名字我叫鲍勃. What's your name I'm Rita. What's your name I'm Nick. 你叫什么名字我叫丽塔. 你叫什么名字我叫尼克. What's your name I'm Lisa. 你叫什么名字我叫利萨. 5. A story-Pit'sskateboard. 5 一个故事-彼德的滑板. Pa:Hello,Pit. Pa:好,彼德. Pi:Hello,:What's this Pi:嗨,帕特.Pa:这是什么 Pi:My new :Look!Pi:Goodbye,Pat! Pi:这是我的新滑板.Pi:看!Pi:再见,帕特! Pa:Bye-bye,Pit!Pi:Help!Help!pi:Bye-bye,skateboard! Pa:再见,彼德!Pi:救命!救命!Pi:再见,滑板! Unit 16. Let's learnand act 第1单元6 我们来边学边表演.
1.塑封整流二极管 序号型号IF VRRM VF Trr 外形 A V V μs 1 1A1-1A7 1A 50-1000V 1.1 R-1 2 1N4001-1N4007 1A 50-1000V 1.1 DO-41 3 1N5391-1N5399 1.5A 50-1000V 1.1 DO-15 4 2A01-2A07 2A 50-1000V 1.0 DO-15 5 1N5400-1N5408 3A 50-1000V 0.95 DO-201AD 6 6A05-6A10 6A 50-1000V 0.95 R-6 7 TS750-TS758 6A 50-800V 1.25 R-6 8 RL10-RL60 1A-6A 50-1000V 1.0 9 2CZ81-2CZ87 0.05A-3A 50-1000V 1.0 DO-41 10 2CP21-2CP29 0.3A 100-1000V 1.0 DO-41 11 2DZ14-2DZ15 0.5A-1A 200-1000V 1.0 DO-41 12 2DP3-2DP5 0.3A-1A 200-1000V 1.0 DO-41 13 BYW27 1A 200-1300V 1.0 DO-41 14 DR202-DR210 2A 200-1000V 1.0 DO-15 15 BY251-BY254 3A 200-800V 1.1 DO-201AD 16 BY550-200～1000 5A 200-1000V 1.1 R-5 17 PX10A02-PX10A13 10A 200-1300V 1.1 PX 18 PX12A02-PX12A13 12A 200-1300V 1.1 PX 19 PX15A02-PX15A13 15A 200-1300V 1.1 PX 20 ERA15-02～13 1A 200-1300V 1.0 R-1 21 ERB12-02～13 1A 200-1300V 1.0 DO-15 22 ERC05-02～13 1.2A 200-1300V 1.0 DO-15 23 ERC04-02～13 1.5A 200-1300V 1.0 DO-15 24 ERD03-02～13 3A 200-1300V 1.0 DO-201AD 25 EM1-EM2 1A-1.2A 200-1000V 0.97 DO-15 26 RM1Z-RM1C 1A 200-1000V 0.95 DO-15 27 RM2Z-RM2C 1.2A 200-1000V 0.95 DO-15 28 RM11Z-RM11C 1.5A 200-1000V 0.95 DO-15 29 RM3Z-RM3C 2.5A 200-1000V 0.97 DO-201AD 30 RM4Z-RM4C 3A 200-1000V 0.97 DO-201AD 2.快恢复塑封整流二极管 序号型号IF VRRM VF Trr 外形 A V V μs （1）快恢复塑封整流二极管 1 1F1-1F7 1A 50-1000V 1.3 0.15-0.5 R-1 2 FR10-FR60 1A-6A 50-1000V 1. 3 0.15-0.5 3 1N4933-1N4937 1A 50-600V 1.2 0.2 DO-41 4 1N4942-1N4948 1A 200-1000V 1.3 0.15-0. 5 DO-41 5 BA157-BA159 1A 400-1000V 1.3 0.15-0.25 DO-41 6 MR850-MR858 3A 100-800V 1.3 0.2 DO-201AD
常用稳压管型号对照——（朋友发的） 美标稳压二极管型号 1N4727 3V0 1N4728 3V3 1N4729 3V6 1N4730 3V9 1N4731 4V3 1N4732 4V7 1N4733 5V1 1N4734 5V6 1N4735 6V2 1N4736 6V8 1N4737 7V5 1N4738 8V2 1N4739 9V1 1N4740 10V 1N4741 11V 1N4742 12V 1N4743 13V 1N4744 15V 1N4745 16V 1N4746 18V 1N4747 20V 1N4748 22V 1N4749 24V 1N4750 27V 1N4751 30V 1N4752 33V 1N4753 36V 1N4754 39V 1N4755 43V 1N4756 47V 1N4757 51V 需要规格书请到以下地址下载， 经常看到很多板子上有M记的铁壳封装的稳压管，都是以美标的1N系列型号标识的，没有具体的电压值，刚才翻手册查了以下3V至51V的型号与电压的对 照值，希望对大家有用 1N4727 3V0 1N4728 3V3 1N4729 3V6 1N4730 3V9
1N4733 5V1 1N4734 5V6 1N4735 6V2 1N4736 6V8 1N4737 7V5 1N4738 8V2 1N4739 9V1 1N4740 10V 1N4741 11V 1N4742 12V 1N4743 13V 1N4744 15V 1N4745 16V 1N4746 18V 1N4747 20V 1N4748 22V 1N4749 24V 1N4750 27V 1N4751 30V 1N4752 33V 1N4753 36V 1N4754 39V 1N4755 43V 1N4756 47V 1N4757 51V DZ是稳压管的电器编号，是和1N4148和相近的，其实1N4148就是一个0.6V的稳压管，下面是稳压管上的编号对应的稳压值，有些小的稳压管也会在管体 上直接标稳压电压，如5V6就是5.6V的稳压管。 1N4728A 3.3 1N4729A 3.6 1N4730A 3.9 1N4731A 4.3 1N4732A 4.7 1N4733A 5.1 1N4734A 5.6 1N4735A 6.2 1N4736A 6.8 1N4737A 7.5 1N4738A 8.2 1N4739A 9.1 1N4740A 10 1N4741A 11 1N4742A 12 1N4743A 13
Join In剑桥小学英语(改编版)入门阶段 Unit 1Hello,hello第1单元嗨,嗨 1.Listen and mime. 1 听,模仿 Stand up Say 'hello' Slap hands Sit down 站起来说"嗨" 拍手坐下来 Good. Let's do itagain.Stand up Say 'hello' Slap hands Sit down 好. 我们来再做一遍.站起来说"嗨"拍手坐下来 2.listen again.Number the pictures. 2 再听一遍给图画编号. 1.Stand up 2.Say "hello" 3.Slap hands 4.Sit down 1 站起来 2 说"嗨" 3 拍手 4 坐下来说 3. A song.Hello,what's yourname? 3 一首歌嗨,你叫什么名字? Hello. Hello.Hello, what's yourname? Hello. Hello. 嗨. 嗨. 嗨, 你叫什么名字? 嗨,嗨. Hello, what's yourname? I'm Toby. I'm Toby. Hello,hello,hello. 嗨, 你叫什么名字? 我叫托比. 我叫托比 . 嗨,嗨,嗨. I'm Toby. I'm Toby. Hello,hello, let's go! 我是托比. 我是托比. 嗨,嗨, 我们一起! Hello. Hello.Hello, what's yourname? I'm Toby.I'm Toby. 嗨.嗨.嗨, 你叫什么名字? 我叫托比.我叫托比. Hello,hello,hello. I'm Toby.I'm Toby. Hello,hello,let's go! 嗨,嗨,嗨.我是托比. 我是托比. 嗨,嗨,我们一起! 4 Listen and stick 4 听和指 What's your name? I'm Bob. 你叫什么名字? 我叫鲍勃. What's your name ? I'm Rita. What's your name ? I'm Nick. 你叫什么名字? 我叫丽塔. 你叫什么名字? 我叫尼克. What's your name ? I'm Lisa. 你叫什么名字? 我叫利萨. 5. A story-Pit'sskateboard. 5 一个故事-彼德的滑板. Pa:Hello,Pit. Pa:好,彼德. Pi:Hello,Pat.Pa:What's this? Pi:嗨,帕特.Pa:这是什么? Pi:My new skateboard.Pi:Look!Pi:Goodbye,Pat! Pi:这是我的新滑板.Pi:看!Pi:再见,帕特! Pa:Bye-bye,Pit!Pi:Help!Help!pi:Bye-bye,skateboard! Pa:再见,彼德!Pi:救命!救命!Pi:再见,滑板! Unit 16. Let's learnand act 第1单元6 我们来边学边表演.
二极管封装大全 篇一：贴片二极管型号、参数 贴片二极管型号.参数查询 1、肖特基二极管SMA（DO214AC） 2010-2-2 16:39:35 标准封装： SMA 2010 SMB 2114 SMC 3220 SOD123 1206 SOD323 0805 SOD523 0603 IN4001的封装是1812 IN4148的封装是1206 篇二：常见贴片二极管三极管的封装 常见贴片二极管/三极管的封装 常见贴片二极管/三极管的封装 二极管： 名称尺寸及焊盘间距其他尺寸相近的封装名称 SMC SMB SMA SOD-106 SC-77A SC-76/SC-90A SC-79 三极管： LDPAK
DPAK SC-63 SOT-223 SC-73 TO-243/SC-62/UPAK/MPT3 SC-59A/SOT-346/MPAK/SMT3 SOT-323 SC-70/CMPAK/UMT3 SOT-523 SC-75A/EMT3 SOT-623 SC-89/MFPAK SOT-723 SOT-923 VMT3 篇三：常用二极管的识别及ic封装技术 常用晶体二极管的识别 晶体二极管在电路中常用“D”加数字表示，如： D5表示编号为5的二极管。 1、作用：二极管的主要特性是单向导电性，也就是在正向电压的作用下，导通电阻很小;而在反向电压作用下导通电阻极大或无穷大。正因为二极管具有上述特性，无绳电话机中常把它用在整流、隔离、稳压、极性保护、编码控制、调频调制和静噪等电路中。 电话机里使用的晶体二极管按作用可分为：整流二极管(如1N4004)、隔离二极管(如1N4148)、肖特基二极管(如BAT85)、发光二极管、稳压二极管等。 2、识别方法：二极管的识别很简单，小功率二极管的N极(负极)，在二极管外表大多采用一种色圈标出来，有些二极管也用二极管专用符号来表示P极(正极)或N极(负极)，也有采用符号标志为“P”、“N”来确定二极管极性的。发光二极管的正负极可从引脚长短来识别，长
五年级下英语月考试卷-全能练考-Join in剑桥英语 姓名：日期：总分：100 一、根据意思，写出单词。（10′） Fanny:Jackie, ________[猜] my animal,my ________最喜欢的 animal.OK? Jackie:Ok!Mm…Has it got a nose? Fanny:Yes,it’s got a big long nose,…and two long ________[牙齿]. Jackie:Does it live in ________[美国]? Fanny:No,no.It lives ________[在] Africa and Asia. Jackie:Can it ________[飞]? Fanny:I’m sorry it can’t. Jackie:Is it big? Fanny:Yes,it’s very big and ________[重的]. Jackie:What ________[颜色] is it?Is it white or ________[黑色]? Fanny:It’s white. Jackie:Oh,I see.It’s ________[大象]. 二、找出不同类的单词。（10′） （）1 A.sofa B.table C.check （）2 A.noodle https://www.doczj.com/doc/ad8361867.html,k C.way （）3 A.fish B.wolf C.lion （）4 A.bike B.car C.write （）5 A.tree B.farm C.grass （）6 A.big B.small C.other ( ）7 A.eat B.listen C.brown
1N 系列常用整流二极管的主要参数
反向工作 峰值电压 URM/V 额定正向 整流电流 整流电流 IF/A 正向不重 复浪涌峰 值电流 IFSM/A 正向 压降 UF/V 反向 电流 IR/uA 工作 频率 f/KHZ 外形 封装
型 号
1N4000 1N4001 1N4002 1N4003 1N4004 1N4005 1N4006 1N4007 1N5100 1N5101 1N5102 1N5103 1N5104 1N5105 1N5106 1N5107 1N5108 1N5200 1N5201 1N5202 1N5203 1N5204 1N5205 1N5206 1N5207 1N5208 1N5400 1N5401 1N5402 1N5403 1N5404 1N5405 1N5406 1N5407 1N5408
25 50 100 200 400 600 800 1000 50 100 200 300 400 500 600 800 1000 50 100 200 300 400 500 600 800 1000 50 100 200 300 400 500 600 800 1000
1
30
≤1
＜5
3
DO-41
1．5
75
≤1
＜5
3
DO-15
2
100
≤1
＜10
3
3
150
≤0.8
＜10
3
DO-27
常用二极管参数： 05Z6.2Y 硅稳压二极管 Vz=6~6.35V,Pzm=500mW,
《剑桥小学英语Join In ——Book 3 下学期》教材教法分析2012-03-12 18:50:43| 分类：JOIN IN 教案| 标签：|字号大中小订阅. 一、学情分析： 作为毕业班的学生，六年级的孩子在英语学习上具有非常显著的特点： 1、因为教材的编排体系和课时不足，某些知识学生已遗忘，知识回生的现象很突出。 2、有的学生因受学习习惯及学习能力的制约，有些知识掌握较差，学生学习个体的差异性，学习情况参差不齐、两级分化的情况明显，对英语感兴趣的孩子很喜欢英语，不喜欢英语的孩子很难学进去了。 3、六年级的孩子已经进入青春前期，他们跟三、四、五年级的孩子相比已经有了很大的不同。他们自尊心强，好胜心强，集体荣誉感也强，有自己的评判标准和思想，对知识的学习趋于理性化，更有自主学习的欲望和探索的要求。 六年级学生在英语学习上的两极分化已经给教师的教学带来很大的挑战，在教学中教师要注意引导学生调整学习方式： 1、注重培养学生自主学习的态度 如何抓住学习课堂上的学习注意力，吸引他们的视线，保持他们高涨的学习激情，注重过程的趣味化和学习内容的简易化。 2、给予学生独立思考的空间。 3、鼓励学生坚持课前预习、课后复习的好习惯。 六年级教材中的单词、句子量比较多，难点也比较多，学生课前回家预习，不懂的地方查英汉词典或者其它资料，上课可以达到事半功倍的效果，课后复习也可以很好的消化课堂上的内容。 4、注意培养学生合作学习的习惯。 5、重在培养学生探究的能力：学习内容以问题的方式呈现、留给学生更多的发展空间。 二、教材分析： （一）.教材特点： 1．以学生为主体，全面提高学生的素质。
1N系列稳压管
快恢复整流二极管
常用整流二极管型号和参数 05Z6.2Y 硅稳压二极管 Vz=6~6.35V,Pzm=500mW, 05Z7.5Y 硅稳压二极管 Vz=7.34~7.70V,Pzm=500mW, 05Z13X硅稳压二极管 Vz=12.4~13.1V,Pzm=500mW, 05Z15Y硅稳压二极管 Vz=14.4~15.15V,Pzm=500mW, 05Z18Y硅稳压二极管 Vz=17.55~18.45V,Pzm=500mW, 1N4001硅整流二极管 50V, 1A,(Ir=5uA,Vf=1V,Ifs=50A) 1N4002硅整流二极管 100V, 1A, 1N4003硅整流二极管 200V, 1A, 1N4004硅整流二极管 400V, 1A, 1N4005硅整流二极管 600V, 1A, 1N4006硅整流二极管 800V, 1A, 1N4007硅整流二极管 1000V, 1A, 1N4148二极管 75V, 4PF,Ir=25nA,Vf=1V, 1N5391硅整流二极管 50V, 1.5A,(Ir=10uA,Vf=1.4V,Ifs=50A) 1N5392硅整流二极管 100V,1.5A, 1N5393硅整流二极管 200V,1.5A, 1N5394硅整流二极管 300V,1.5A, 1N5395硅整流二极管 400V,1.5A, 1N5396硅整流二极管 500V,1.5A, 1N5397硅整流二极管 600V,1.5A, 1N5398硅整流二极管 800V,1.5A, 1N5399硅整流二极管 1000V,1.5A, 1N5400硅整流二极管 50V, 3A,(Ir=5uA,Vf=1V,Ifs=150A) 1N5401硅整流二极管 100V,3A, 1N5402硅整流二极管 200V,3A, 1N5403硅整流二极管 300V,3A, 1N5404硅整流二极管 400V,3A,
常用稳压二极管技术参数及老型号代换 型号最大功耗 (mW) 稳定电压(V) 电流(mA) 代换型号国产稳压管日立稳压管 HZ4B2 500 3.8 4.0 5 2CW102 2CW21 4B2 HZ4C1 500 4.0 4.2 5 2CW102 2CW21 4C1 HZ6 500 5.5 5.8 5 2CW103 2CW21A 6B1 HZ6A 500 5.2 5.7 5 2CW103 2CW21A HZ6C3 500 6 6.4 5 2CW104 2CW21B 6C3 HZ7 500 6.9 7.2 5 2CW105 2CW21C HZ7A 500 6.3 6.9 5 2CW105 2CW21C HZ7B 500 6.7 7.3 5 2CW105 2CW21C HZ9A 500 7.7 8.5 5 2CW106 2CW21D HZ9CTA 500 8.9 9.7 5 2CW107 2CW21E HZ11 500 9.5 11.9 5 2CW109 2CW21G HZ12 500 11.6 14.3 5 2CW111 2CW21H HZ12B 500 12.4 13.4 5 2CW111 2CW21H HZ12B2 500 12.6 13.1 5 2CW111 2CW21H 12B2 HZ18Y 500 16.5 18.5 5 2CW113 2CW21J HZ20-1 500 18.86 19.44 2 2CW114 2CW21K HZ27 500 27.2 28.6 2 2CW117 2CW21L 27-3 HZT33-02 400 31 33.5 5 2CW119 2CW21M RD2.0E(B) 500 1.88 2.12 20 2CW100 2CW21P 2B1 RD2.7E 400 2.5 2.93 20 2CW101 2CW21S RD3.9EL1 500 3.7 4 20 2CW102 2CW21 4B2 RD5.6EN1 500 5.2 5.5 20 2CW103 2CW21A 6A1 RD5.6EN3 500 5.6 5.9 20 2CW104 2CW21B 6B2 RD5.6EL2 500 5.5 5.7 20 2CW103 2CW21A 6B1 RD6.2E(B) 500 5.88 6.6 20 2CW104 2CW21B RD7.5E(B) 500 7.0 7.9 20 2CW105 2CW21C RD10EN3 500 9.7 10.0 20 2CW108 2CW21F 11A2 RD11E(B) 500 10.1 11.8 15 2CW109 2CW21G RD12E 500 11.74 12.35 10 2CW110 2CW21H 12A1 RD12F 1000 11.19 11.77 20 2CW109 2CW21G RD13EN1 500 12 12.7 10 2CW110 2CW21H 12A3 RD15EL2 500 13.8 14.6 15 2CW112 2CW21J 12C3 RD24E 400 22 25 10 2CW116 2CW21H 24-1
五 年 级 英 语 测 试 卷 学校 班级 姓名 听力部分（共20分） 一、Listen and colour . 听数字，涂颜色。（5分） 二、 Listen and tick . 听录音，在相应的格子里打“√”。 （6分） 三、Listen and number.听录音，标序号。（9分） pig fox lion cow snake duck
sheep 笔试部分（共80分） 一、Write the questions.将完整的句子写在下面的横线上。(10分) got it Has eyes on a farm it live sheep a it other animals eat it it Is 二、Look and choose.看看它们是谁，将字母填入括号内。(8分) A. B. C. D.
E. F. G. H. ( ) pig ( ) fox ( ) sheep ( ) cat ( ) snake ( ) lion ( ) mouse ( ) elephant 三、Look at the pictures and write the questions.看图片，根据答语写出相应的问题。(10分) No,it doesn’t. Yes,it is.
Yes,it does. Yes,it has. Yes,it does. 四、Choose the right answer.选择正确的答案。(18分) 1、it live on a farm？ 2. it fly？
3. it a cow？ 4. it eat chicken？ 5. you swim？ 6. you all right？ 五、Fill in the numbers.对话排序。(6分) Goodbye. Two apples , please. 45P , please. Thank you.
常用稳压管型号参数对照 3V到51V 1W稳压管型号对照表1N4727 3V0 1N4728 3V3 1N4729 3V6 1N4730 3V9 1N4731 4V3 1N4732 4V7 1N4733 5V1 1N4734 5V6 1N4735 6V2 1N4736 6V8 1N4737 7V5
1N4739 9V1 1N4740 10V 1N4741 11V 1N4742 12V 1N4743 13V 1N4744 15V 1N4745 16V 1N4746 18V 1N4747 20V 1N4748 22V 1N4749 24V 1N4750 27V 1N4751 30V
1N4753 36V 1N4754 39V 1N4755 43V 1N4756 47V 1N4757 51V 摩托罗拉IN47系列1W稳压管IN4728 3.3v IN4729 3.6v IN4730 3.9v IN4731 4.3 IN4732 4.7 IN4733 5.1
IN4735 6.2 IN4736 6.8 IN4737 7.5 IN4738 8.2 IN4739 9.1 IN4740 10 IN4741 11 IN4742 12 IN4743 13 IN4744 15 IN4745 16 IN4746 18 IN4747 20
IN4749 24 IN4750 27 IN4751 30 IN4752 33 IN4753 34 IN4754 35 IN4755 36 IN4756 47 IN4757 51 摩托罗拉IN52系列 0.5w精密稳压管IN5226 3.3v IN5227 3.6v
2011-2012 学年度上学期六年级复习题（Unit2-Unit3 ） 一、听力部分 1、听录音排序 ( ) () ()() () 2、听录音，找出与你所听到的单词属同一类的单词 （） 1. A. spaceman B. pond C . tiger （） 2. A.mascots B. potato C . jeans （） 3. A. door B. behind C . golden （） 4. A. sometimes B. shop C . prince （） 5. A. chair B. who C . sell 3、听录音，将下面人物与他的梦连线 Sarah Tim Juliet Jenny Peter 4、听短文，请在属于Mr. Brown的物品下面打√ ( ) ( ) ( ) ( ) ( ) ( ) ( ) 5、听问句选答句 （） 1. A. Yes, I am B. Yes, I have C . Yes, you do （） 2. A.Pink B. A friendship band C . Yes. （） 3. A. OK B. Bye-bye. C . Thanks, too. （） 4. A. Monday. B. Some juice. C . Kitty. （） 5. A. I ’ve got a shookbag. B. I ’m a student. C . It has got a round face. 6、听短文，选择正确答案 （） 1. Where is Xiaoqing from? She is from . A.Hebei B. Hubei C . Hunan （） 2. She goes to school at . A.7:00 B.7:30 C . 7:15 （） 3. How many classes in the afternoon? classes. A. four B. three C . two （） 4. Where is Xiaoqing at twelve o ’clock? She is . A. at home B. at school C .in the park （） 5. What does she do from seven to half past eight? She . A.watches TV B. reads the book C. does homework
Starter Unit Good to see you again知识总结 一. 短语 1. dance with me 和我一起跳舞 2. sing with me 和我一起唱歌 3. clap your hands 拍拍你的手 4. jump up high 高高跳起 5.shake your arms and your legs晃晃你的胳膊和腿 6. bend your knees 弯曲你的膝盖 7. touch your toes 触摸你的脚趾8. stand nose to nose鼻子贴鼻子站 二. 句子 1. ---Good morning. 早上好。 ---Good morning, Mr Li. 早上好，李老师。 2. ---Good afternoon. 下午好。 ---Good afternoon, Mr Brown. 下午好，布朗先生。 3. ---Good evening，Lisa. 晚上好,丽莎。 ---Good evening, Bob. 晚上好，鲍勃。 4. ---Good night. 晚安。 ----Good night. 晚安。 5. ---What’s your name? 你叫什么名字？ ---I’m Bob./ My name is Bob. 我叫鲍勃。 6. ---Open the window, please. 请打开窗户。 ---Yes ,Miss. 好的，老师。 7. ---What colour is it? 它是什么颜色？ 它是蓝红白混合的。 ---It’s blue, red and white. 皮特的桌子上是什么？ 8. ---What’s on Pit’s table? ---A schoolbag, an eraser and two books. 一个书包，一个橡皮和两本书。 9. ---What time is it? 几点钟？ 两点钟。 ---It’s two. 10.---What’s this? 这是什么？ ---My guitar. 我的吉他。