a r X i v :a s t r o -p h /0702442v 1 16 F e
b 2007
Characterizing the disk around the TW Hydrae Association
brown dwarf 2MASSW J1207334-393254
Basmah Riaz and John E.Gizis
Department of Physics and Astronomy,University of Delaware,Newark,DE 19716;
basmah@https://www.doczj.com/doc/fe15727025.html,,gizis@https://www.doczj.com/doc/fe15727025.html,
ABSTRACT
We present detailed modeling of the disk around the TW Hydrae Association
(TWA)brown dwarf 2MASSW J1207334-393254(2M1207),using Spitzer obser-
vations from 3.6to 24μm.The spectral energy distribution (SED)does not show
a high amount of ?aring.We have obtained a good ?t using a ?at disk of mass between 10?4and 10?6M ⊙,˙M
10?11M ⊙yr ?1and a large inclination angle between 60?and 70?.We have used three di?erent grain models to ?t the 10μm
Si emission feature,and have found the results to be consistent with ISM-like
dust.In comparison with other TWA members,this suggests lesser dust pro-
cessing for 2M1207which could be explained by mechanisms such as aggregate
fragmentation and/or turbulent mixing.We have found a good ?t using an inner
disk radius equal to the dust sublimation radius,which indicates the absence of
an inner hole in the disk.This suggests the presence of a small K-L ′excess,
similar to the observed K-[3.6]excess.
Subject headings:accretion,accretion disks –circumstellar matter –stars:low-
mass,brown dwarfs –stars:individual (2MASSW J1207334-393254)1.Introduction
Over the last decade,a large number of sub-stellar mass objects have been discovered,
with masses ranging from the hydrogen burning limit ( 0.075M ⊙)down to the mass of giant planets and below the deuterium burning limit ( 0.013M ⊙).The presence of accretion disks in sub-stellar objects has been con?rmed by signatures of ongoing accretion (e.g.Muzerolle et al.2003,2005;Mohanty et al.2005)and the presence of excess emission in the near-and mid-infrared (e.g.Jayawardhana et al.2003;Muench et al.2001;Mohanty et al.2004;Apai et al.2004;Luhman et al.2005).The fraction of circumstellar disks appears to be similar for young brown dwarfs and T Tauri stars (e.g.Luhman et al.2005;
Jayawardhana et al.2003).Furthermore,brown dwarf disks have been found to show a range in disk properties,similar to T Tauri disks.The observed SEDs have been well?t by models of both?ared and?at disks using a range of grain sizes from ISM-like dust to grains as large as1mm(e.g.Allers et al.2006;Muzerolle et al.2006).Inner holes of a few sub-stellar radii have been found to be common in brown dwarf disks(e.g.Mohanty et al. 2004;Allers et al.2006).Recently,Muzerolle et al.(2006)have reported the?rst brown dwarf with evidence of an AU-scale inner disk hole.The inner disk lifetimes for brown dwarf disks appear to be similar to the disks around T Tauri stars(Jayawardhana et al.2003). While some brown dwarfs demonstrate an absence of the silicate emission feature near10μm (e.g.Cha Hα2;Apai et al.2002),others display a variety in the shape and strength of this feature,that have been explained by the presence of either small ISM grains(e.g.Cha Hα1; Sterzik et al.2004)or large amorphous grains of sizes～2μm(e.g.CFHT BD Tau4;Apai et al.2004).Disk masses in the range-4 log(M d/M⊙) -7have been determined for young brown dwarf disks(e.g.Walker et al.2004),with no change seen in the relative disk mass with object mass at the substellar boundary(Scholz et al.2006).A similar absence of discontinuity has been seen in the distribution of disk accretion rates with stellar mass (Muzerolle et al.2005).Together such similarities indicate that brown dwarf disks are just scaled-down versions of T Tauri disks.
A detailed study of brown dwarf disks is important to test the di?erent formation mechanisms for these sub-stellar objects.The numerical simulations of star formation by Bate et al.(2003)have shown that for brown dwarfs that form via the ejection mechanism, i.e.,as stellar embryos in multiple systems that are ejected at an early stage,disks of radii larger than～20AU are rare(～5%).This is because brown dwarfs are ejected so soon after their formation that they do not have time to accrete the high angular momentum gas required to form a large disk.On the other hand,if most brown dwarf disks observed have large outer radii,it would suggest that the ejection mechanism rarely operates and would support a star-like formation,i.e.via the collapse of molecular cloud cores with sub-stellar masses.Planet-like formation of a brown dwarf in a circumstellar disk would,however, require an absence of dust around it(e.g.Apai et al.2002).Recent e?orts by Scholz et al. (2006)have shown that25%of their target brown dwarfs have disk radii>10AU,indicating star-like formation.Observations of larger samples of sub-stellar disks would be able to con?rm or reject the di?erent formation scenarios.Characterization of brown dwarf disks is also important to understand the conditions under which planets can form in these disks. Processes that may lead to planet formation such as grain growth,crystallization and dust settling have been reported for some brown dwarfs(e.g.Apai et al.2005),suggesting that even sub-stellar disks of a few Jupiter masses can harbor planets.
The brown dwarf2MASSW J1207334-393254(hereafter,2M1207)was discovered by
Gizis(2002)and was con?rmed to be a TW Hydrae Association(TWA)member by Scholz, R.-D.et.al.(2005),based on its proper motion.It is known to be undergoing accretion that varies by a factor of5-10on a time scale of～6weeks(Scholz et al.2005).Excess emission has been detected in the infrared(IR)by Sterzik et al.(2004;hereafter S04)and Riaz et al.(2006;hereafter R06),indicating the presence of a circumsubstellar disk of gas and dust.The UV spectrum for2M1207shows H2emission lines as due to the presence of circumsubstellar gas,that gets(shock)heated up to high temperatures of～105K as it falls along an accretion column onto the substellar surface,giving rise to C IV lines in emission (Gizis et al.2005).Gizis et al.had also shown that the lack of Si emission in the hot spots is due to its depletion into dust grains in the circumsubstellar disk.Indeed,observations by S04indicated the presence of Si emission in the dusty disk.Based on their8.7and10.4μm observations,S04had found that both a large grain size(up to5μm),large inclination angle ?ared disk,and a?at disk composed of small(0.1μm)or large(2μm)grains provide a good ?t.In R06,we had reported on the Spitzer observations of2M1207from3.6to24μm,and had shown the presence of warm(T>100K)dust close(R<0.2AU)to the brown dwarf. We were able to get a good?t to our observations using a straight line of slope of～-1.3, indicating a?at disk for2M1207.Here we have used disk models to further characterize the disk.
2.Disk modeling
We have used the2-D radiative transfer code by Whitney et al.(2003).The circum-stellar geometry consists of a rotationally?attened infalling envelope,bipolar cavities,and a ?ared accretion disk in hydrostatic equilibrium.With evolution from a Class0to Class III source,the cavity density and the envelope infall rate decreases,while the disk radius and the cavity opening angle increases.The disk density is proportional to??α,where?is the radial coordinate in the disk midplane,andαis the radial density exponent.The disk scale height increases with radius,h=h0(?/R?)β,where h0is the scale height at R?andβis the?aring power.Since we are?tting a disk source,the envelope was turned o?by setting its mass infall rate equal to zero.For the stellar parameters,we have used T eff=2550K and M?=0.024M⊙(Mohanty et al.2006).Mohanty et al.have considered an age of5-10Myr to determine the https://www.doczj.com/doc/fe15727025.html,ing this T eff and M?,the evolutionary tracks by Burrows et al. (1997)imply R?～0.024R⊙.A distance of59pc(Song et al.2006)was used to scale the output?uxes from the models to the luminosity and distance of2M1207.The NextGen (Hauschildt et al.1999)atmosphere?le for a T eff of2600K,and log g=3.5was used to ?t the atmosphere spectrum of the central sub-stellar source.We note that Mohanty et al.have determined the e?ective temperature by using the DUSTY models by Allard et al.
(2001).However,we could not?nd any di?erences between the two atmospheric models at a T eff of2600K.As noted by Gorlova et al.(2003),variations in these models due to the inclusion of dust opacities become apparent only below～2300K.Table1lists the IRAC and MIPS observations from R06.Table2lists the stellar parameters used,and the range of disk parameters that provide good?ts to2M1207.
Fig.1compares the amount of?aring in2M1207disk with other brown dwarf disks,by looking at the ratio of24and4.5μm?uxes as a function of the24μm?ux.The dashed line represents a geometrically thin,optically thick?at disk with a spectral slopeλFλ∝λ?4/3. The solid line represents the photosphere of a brown dwarf at T eff=2600K.L1707and L291 are two brown dwarf disks in IC348that show some amount of?aring,and have been?t by a model disk with˙M=10?11M⊙yr?1,a max=0.25μm and an inclination of60?(Muzerolle et al.2006).2M1139511-315921(hereafter,2M1139),another brown dwarf in TWA,is nearly photospheric,while TW Hya has a highly?ared disk.2M1207lies just at the dashed line, indicating an optically thick?at disk.That the disk is optically thick can also be inferred from the3.6to8μm slope,α,of the https://www.doczj.com/doc/fe15727025.html,da et al.(2006)have used the values ofαto discriminate between sources with and without disks in IC348.Sources withα>-1.8have optically thick disks,while the ones with-1.8>α>-2.65have anemic or optically thin disks.A source withα<-2.56is photospheric(i.e.disk-less).Anαof-1.5for2M1207thus indicates the presence of an optically thick disk.
For a disk in vertical hydrostatic equilibrium,the amount of?aring in the disk depends on the stellar mass and the disk temperature,as the disk scale height h∝(T d/M?)1/2(Walker et al.2004).Thus the scale height increases with decreasing mass,resulting in more vertically extended disks for brown dwarfs compared to those around classical T Tauri stars(CTTS). Walker et al.found h(100AU)for a0.01M⊙brown dwarf to be～60AU,compared to～15 AU for a CTTS.Due to the larger scale heights for lower masses,the disk can intercept and thus scatter and reprocess more stellar radiation,resulting in large infrared excesses.We have varied the degree of?aring by adjusting the values of the?aring powerβ.Fig.2a shows that for M2M1207～0.024M⊙,the SED is highly?ared forβ=1.25(typical value for models of T Tauri disks in hydrostatic equilibrium).The variations in the SEDs asβis lowered are more evident forλ>10μm.Our24μm observation indicates that the models withβbetween1.05and1.1are good?ts to2M1207disk.
The models we are using here consider a?ared accretion disk.Walker et al.(2004) have shown that low mass?ared disks are a good?t to SEDs that had been previously ?t by a?at disk.Even though the hydrostatic solution gives a highly?ared disk,most of the mass is in the gas due to a gas-to-dust mass ratio of100.So if there is dust settling in a?ared disk,the dust disk observed in the IR could still be?attened compared to the
gas disk.Walker et al.have concluded that long wavelength observations are required to discriminate between a?at disk and a low mass?ared disk.The typical range of brown dwarf disk masses is found to be-4 log(M d/M⊙) -7(e.g.Walker et al.2004,Scholz et al.2006).In Fig.2b,we have varied the disk masses between10?2M⊙and10?9M⊙.Higher mass disks are more?ared,while the10?9M⊙SED is nearly photospheric.As the disk mass decreases,the disk becomes optically thin,and near and mid-infrared radiation is seen from the whole disk,whereas for larger disk masses,the disk is optically thick and IR radiation is only seen from the surface layers of the disk.Variations in the SEDs are more evident for λ>10μm,and our24μm observation indicates disk masses between10?4and10?6M⊙to be good?ts.Observations at far-IR/sub-mm wavelengths can correctly determine the disk mass and con?rm the presence of a population of large grains that dominate the disk mass but contribute little to the opacity at near-and mid-IR wavelengths.
In Fig.2c,we have explored a range of inclination angles to the line of sight.Due to binning of photons in the models,there are a total of10viewing angles,with face-on covering0-18?inclinations.The mid-and far-IR?uxes increase with decreasing inclinations, as the emission at these wavelengths is from an optically thick disk,while the optically thin millimeter?uxes are independent of the inclination.For edge-on disks,the star contributes only indirectly through scattered light.The10μm silicate feature is a broad absorption band for such sources,since the large extinction in the disk midplane blocks thermal radiation from the deeper layers,and low albedos prevent radiation from scattering out through the upper disk layers(Whitney et al.2003).Fig.2c shows that bins of63?and69?are a good?t to 2M1207disk.On the basis of the redshifted absorption component in the Hαpro?le,Scholz et al.(2005)had concluded that2M1207is seen with an inclination of i 60?.Our model ?ts are thus consistent with previous conclusion on the inclination angle.
A well-mixed model assumes di?use ISM-like dust(i.e.silicates and graphite grains with a maximum size of～0.25μm)to be uniformly mixed with the disk gas.However, such models exhibit too little mm-?ux and larger far-infrared?uxes than those observed for CTTS(D′Alessio et al.2006).Indeed,Scholz et al.(2006)could not?nd a good?t to their Taurus brown dwarf disks using models with dust and gas well mixed in vertical hydrostatic equilibrium,as these produce too large far-infrared emission,while underpredict the mid-infrared?uxes.The?at SED slopes observed at mm-wavelengths in some T Tauri disks indicate the presence of grains larger than those in the ISM.This suggests dust settling and grain growth that a?ect disk temperatures and vertical structures,resulting in dust photospheres that are?atter rather than?ared(e.g.,Dullemond&Dominik2004).With grain evolution,the upper disk layers are rapidly depleted of the dust material,leaving only the smallest grains at larger scale heights while the larger grains settle in the disk midplane. With reduction in number of small grains in the upper layers,the IR opacity decreases,which
results in lower IR?uxes.Also,this small population of small grains at larger scale heights produces the observed emission features such as the silicate bands near10μm.The large grains that settle in the interior are able to produce large mm?uxes(due to their larger mm emissivity)and can explain the observed?at SED slopes at mm wavelengths(D′Alessio et al.2006).Thus models in which grain sizes vary with the scale height in the disk are better able to?t the observed SEDs,compared to the well-mixed models.
The models used here provide the capability to include di?erent grains in di?erent regions(see Whitney et al.2003,Fig.1).There are three grain models supplied by the code.All of these grain models use a range of grain sizes that can be approximated as a power-law.The di?erence is in the maximum grain sizes.The three grain models used are: large grains with a size distribution that decays exponentially for sizes larger than50μm up to1mm,grains of sizes with a max～1μm,and ISM-like grains with a max～0.25μm.We have varied these three di?erent grain sizes in the disk midplane and the upper atmosphere. The upper atmosphere corresponds to the highest layers in the disk,while the disk midplane is the densest region.The code,by default,uses the large grains of a max=1mm in the disk midplane,the a max～1μm grains in the disk atmosphere,and the ISM-like grains in the out?ow.In short,the grain size decreases with increasing scale height in the disk,with the small grains in the upper layers and large grains in the midplane.
Using these default parameters,while the model SED is a good?t to our IRAC and24μm observations(Fig.3a),it fails to produce the silicate emission feature near10μm,as can be seen from Fig.3b.Wavelengths between7and14μm cover the10μm silicate emission feature,whose shape and strength is determined by dust grain size and composition.A peak at9.8μm indicates the presence of amorphous interstellar grains,while disks that show prominent crystalline silicate emission features,indicative of highly processed dust,have characteristic peaks at9.3and11.3μm(e.g.,Apai et al.2005).For the case of2M1207, there are only three observations(at8,8.7and10.4μm)in this wavelength range to indicate the presence of a silicate emission feature.We have used a simple reducedχ2analysis to determine if the large or the small grains provide a good?t to this feature.Fig.3b shows that if the disk midplane grain model is changed from a max=1mm to the a max～1μm sized grains,the SED is a good?t to the8.7μm observation,but the?uxes are still low to?t the10.4μm point.On the other hand,reducing the grain size further to ISM-type grains with a max～0.25μm provides the best?t(lowest reducedχ2value)to the silicate feature. For our IRAC and24μm observations,any grain model provides a good?t,as variations in the SEDs for di?erent grain sizes are evident at either～10μm or at far-IR/sub-mm wavelengths.The presence of large grains in the disk midplane results in?atter slopes at longer wavelengths,as can be seen from Fig.3a.
The changes in the grain sizes discussed above were made in the disk midplane,while setting the disk atmosphere grains to sizes of a max～1μm.We next varied the disk upper atmosphere grain sizes,while setting the disk midplane grains to a max～1mm.In the disk atmosphere,using ISM-like grains or any other grain size fails to produce the silicate emission feature.The10μm silicate feature only seems to be sensitive to the grains in the disk midplane.This can be explained by the di?erence in theτ=1surface depth as a function of wavelength of the emission.Though the10μm silicate feature arises from the optically thin surface layer of the disk,it probes a deeper layer compared to shorter wavelengths.The upper atmosphere corresponds to the highest layers of the disk,where the disk material is optically thick toλ～1μm stellar radiation.Atλ～10μm,characteristic of the reprocessed radiation from the top disk layers,the disk has less optical depth and the reprocessed radiation can di?use and heat up the inner layers of the disk.The disk atmosphere is heated up to a higher temperature than the inner layers,resulting in a vertical temperature inversion that produces the silicate feature in emission(Calvet et al.1992).The model used here assigns large grains to the high density regions.Due to this,when large grains are used in the disk midplane,similar grains are placed close to the inner wall since it is of high density.This a?ects the emission from the inner wall and hence the observed?ux at10μm.Thus by using sub-micron sized grains in the disk midplane,we have indirectly reduced the inner wall grain size,and were able to obtain a good?t to the10μm Si feature. There could still be bigger grains in the really dense midplane region of the disk,the presence of which can be con?rmed with far-IR/sub-mm observations.On the other hand,if this were a′′three-layered′′disk model instead of a′′two-layered′′one,large grains could be placed in the very dense regions without a?ecting the10μm feature.
On the basis of a reducedχ2analysis,we have found that ISM-like grains provide the best?t to the10μm silicate emission feature for2M1207.This is in contrast with other TWA members,such as TW Hya,HD98800B and Hen3-600A,that exhibit broad silicate emission features.The N-band spectra for Hen3-600A shows a mixture of crystalline silicate components(Honda et al.2003),while those for TW Hya and HD98800B have been?t using large(2μm)amorphous olivine grains(Weinberger et al.2002,Sch¨u tz et al.2004).Grain growth and crystallization have similar e?ects on the10μm silicate feature(Kessler-Silacci et al.2006).As grains grow from sub-micron sizes to several microns,the10μm feature becomes weaker and less peaked.2M1207shows weak dust processing signatures compared to other TWA members.The presence of grain growth and settling in other brown dwarfs (e.g.,Apai et al.2005)does not support di?erent dust processing mechanisms for stellar and sub-stellar objects.However,if mechanisms such as aggregate fragmentation and/or turbulent mixing occur along with grain growth in the disk,then the time scales over which grain growth and dust settling takes place may be prolonged.Fragmentation results in
replenishment of small grains throughout the disk,while turbulent mixing can increase the time scale over which grains settle,as it can bring both large and small grains back to the disk surface.Grain growth models by Dullemond&Dominik(2004)indicate that growth to meter sizes is rapid(～103years at1AU and105years at30AU).On the other hand, fragmentation of grains allows for a semi-stationary state to be reached after about104years, for grain sizes below～1cm,which may last for several million years.Thus an equilibrium between grain growth and small grain replenishment rates may explain the presence of ISM-type grains in the upper disk layers of2M1207at an age of～10Myr.Due to the regeneration of small grains on the disk surface,Kessler-Silacci et al.(2006)could not?nd a correlation between the strength of the10μm feature and the age or disk evolutionary state,which is consistent with our?nding of weaker dust processing in2M1207compared to other TWA members.However,a detailed study of the N-band spectrum for2M1207would make it possible to decompose the10μm feature into distinct dust species and con?rm our results.
The above analysis of grain sizes is based on the10μm silicate feature.The?at slopes of the SED at millimeter wavelengths can correctly indicate the presence of grains larger than those in the ISM.As shown in Fig.3a,using sub-micron sized particles in the disk midplane provides a good?t to our observations up to24μm.This results in steeper slopes at sub-millimeter wavelengths.Lommen et al.(2006)have found a correlation between the peak10μm?ux and the millimeter slope for T Tauri disks,indicating that grain growth occurs in the outer disk and in the surface layers of the inner disk simultaneously.They have explained that when aggregates are fragmented in collisions,which must take place in order to preserve the small grain population in the upper disk layers to produce the10μm feature,the size of the fragments increases as the aggregate size increases.That is,larger particles are produced due to fragmentation of larger aggregates.For the case of TW Hya, the outer disk is optically thick and requires～1cm sized particles to?t the sub-millimeter and millimeter slopes,while the inner disk region of 4AU is optically thin,and requires ～1μm sized grains to produce the silicate feature(Calvet et al.2002).The presence of sub-micron sized particles in the upper layers of2M1207disk,as indicated by model?ts, then suggests that the largest particles in the disk have not yet grown to sizes of millimeter or larger,indicating steeper slope in the millimeter regime.
Fig.4a shows the SEDs for mass accretion rates between10?9and10?12M⊙yr?1. Higher accretion rates result in larger scale heights in the optical and far-IR,but lower at near-IR wavelengths.Typical˙M values for young low mass stars and brown dwarfs are in the range of10?10and10?12M⊙yr?1(Muzerolle et al.2005).Mohanty et al.(2003)have con?rmed2M1207to be a CTTS-like accretor on the basis of the detection of He I and upper Balmer lines and the condition that accretors should display broad asymmetric Hαemission. Scholz et al.(2005)have found that the accretion rate varies by a factor of5-10between
10?10.1±0.7and10?10.8±0.5M⊙yr?1,on a timescale of6weeks.Fig.4a shows that while the SED for10?9M⊙yr?1is clearly not a good?t,˙M of10?10M⊙yr?1indicates excess emission in the optical and UV.The hot continuum emission seen in the optical and the ultraviolet wavelengths is produced by the accretion energy dissipated when the hot gas shocks at the stellar surface(Hartmann2000).We have included in Fig.4a the photographic magnitudes B and R from the SuperCOSMOS Sky Survey(magnitudes obtained from Scholz,R.-D.et al.2005).Though the errors for these magnitudes are large,including them rules out the model?t for10?10M⊙yr?1.On the other hand,model SEDs for˙M of10?11and10?12M⊙yr?1provide a good?t.Thus with the available observations,our model?ts are consistent with the lower value of accretion rate of～10?10.8M⊙yr?1reported by Scholz et al.However, the presence of C IV lines in emission in the UV spectrum(Gizis et al.2005),that are formed when hot gas of～105K falls along an accretion column onto the substellar surface,and the strong evidence of funneled rather than spherical accretion(Scholz et al.2005),indicates the presence of continuum excess emission in the optical and UV bands for2M1207,which needs to be con?rmed with future observations.
Fig.4b shows the separate contributions of the inner rim(wall)at the dust sublimation radius(discussed below),the disk truncated at this radius,the stellar photosphere and the scattered?ux,for a disk of mass10?5M⊙,inclination of63?and˙M of10?11M⊙yr?1.The disk models include the emission from the inner rim.In order to determine its separate contribution,we have calculated the inner rim?uxes using equations in Dullemond et al. (2001).As discussed above,contribution from the scattered light increases as the disk becomes more inclined,such that it can account for up to90%of the K-band?ux for an edge-on disk(Walker et al.2004).The inner rim is a major contributor to?uxes shortward of10μm,and dominates the excess seen above the photosphere at shorter wavelengths.The ?ux at10μm is a sum of emission from the disk and the inner rim.The outer regions of the disk contribute more?ux at longer wavelengths.The fractional disk luminosity for2M1207 is found to be0.03.This is higher than TWA7and13for which cool debris disks have been detected at70μm(Low et al.2005).Other prominent stellar members in TWA like TW Hya,Hen3-600and HD98800B have larger L IR/L?of the order of0.2due to their strong excesses at mid-and far-IR wavelengths.
The inner disk radius,R in,was set to1R sub,where R sub is the dust sublimation radius and varies with the stellar radius and temperature,R sub=R?(T sub/T?)?2.085(Whitney et al.2003).T sub is the dust sublimation temperature and was set to1600K.For2M1207, 1R sub～3R?.Fig.4c shows the variations in the model SEDs with increasing R in.We have obtained good?ts for R in between1and3R sub,with a peak at1R sub(based on a reduced χ2comparison).Increasing the inner radius to5or7R sub results in higher?uxes near the 10μm silicate band and at longer wavelengths.Inner holes of a few sub-stellar radii(～3to
7R?)are found to be common around brown dwarfs(e.g.Allers et al.2006;Mohanty et al. 2004).On the basis of a lack of a K-L′excess,Jayawardhana et al.(2003)suggested an inner hole in2M1207disk.However,we have obtained the best?t for R in=1R sub,which implies an absence of an inner disk hole since it would have to be larger than the dust sublimation radius.This suggests the presence of some K-L′excess.Since the disk is relatively?at,the K-L′excess will be small,similar to the observed K-[3.6]excess,even if the inner radius extends down to the dust sublimation radius.Jayawardhana et al.have used a conservative limit of K-L′ 0.2to de?ne this excess,which may be the reason for their observation to be purely photospheric.Other than TW Hya,Hen3-600,HD98800B and HR4796A,most of the TWA members do not show any excess at near-and mid-IR wavelengths,which indicates dissipation of dusty inner disks on a time scale of 10Myr(Low et al.2005;Jayawardhana et al.1999).The lack of inner disk dissipation for2M1207could be explained by a possible non-coevality in the TWA.There are results suggesting two distinct populations in TWA, as evidenced by a bimodal distribution in the rotation periods(Lawson&Crause2005)and the presence of warm(T 100K)dust(Low et al.2005;Weinberger et al.2004).Low et al.found negligible amounts of warm dust around20out of their24TWA targets,while the other four(mentioned above)display strong excess emission at24μhttps://www.doczj.com/doc/fe15727025.html,wson&Crause have found the median rotation period for the TWA1-13group led by TW Hya to be4.7d, while that for the stars in the TWA14-19group to be0.7d.These authors have suggested that the former group might be younger than the latter by～8Myr(8-10Myr versus～17 Myr).An upper period limit of25hr for2M1207(Scholz et al.2005)would then place it closer to the older(～17Myr)group.Recently,Barrado y Navascu′e s(2006)has estimated
Myr.Considering the large uncertainty in this estimate,if the age for2M1207to be15+15
?10
2M1207is indeed as young as～5Myr,this would explain the lack of inner disk evolution in this brown dwarf disk.On the other hand,if it is as old as～30Myr,then regeneration of small grains in the upper disk layers would be a plausible explanation for the lack of inner disk clearing,as discussed above.Given the assumption that all TWA members have similar ages,the wide variety in the SEDs is similar to what has been observed for T Tauri disks in other https://www.doczj.com/doc/fe15727025.html,da et al.(2006)found that the IR excess due to circumstellar disks around low-mass stars in the IC348cluster(2-3Myr)ranges from optically thick?ared disks to diskless photospheres.Hartmann et al.(2005)found a similar variety in the SEDs of CTTS in Taurus(0.1-2Myr).These vary from stars with highly?ared disks(e.g.,DR Tau),to transitional disks(e.g.,GM Aur)and stars with purely photospheric emission(e.g., IW Tau).The di?erences in the SEDs are attributed to the variations in the scale heights of the disks as well as the disk inclinations and disk masses,but could also be re?ecting intrinsic di?erences in the star systems themselves,such as di?erent initial conditions or other intrinsic properties like the activity level of the star,or planet formation,etc.
We have varied the outer disk radius between5and200AU.Since the disk mass was ?xed at10?5M⊙,smaller R out resulted in larger optical depth.However,the changes in the SEDs are more evident at far-IR/sub-mm wavelengths,and longer wavelength observations can correctly determine the outer disk radius.As discussed in the introduction,Bate et al.(2003)have predicted truncated disks of outer radii<10-20AU,if brown dwarfs form via the ejection scenario.Though we have obtained a good?t using R out=100AU,the degeneracies in our?ts do not allow us to rule out such a formation scenario for2M1207. We are able to get similar?ts by varying both disk mass and outer radius to give similar optical depths at the wavelengths being modeled.As discussed in Walker et al.(2004),it is di?cult to test such predictions with SEDs alone,and high resolution imaging is required to resolve the disk via their scattered and thermal emission.
3.Summary
Due to the large number of free parameters and the absence of longer wavelength ob-servations,there are degeneracies in the model?ts presented here.The uncertainties in the stellar parameters could also result in changes in the disk parameters.Nevertheless, our model?ts indicate that grain sizes of a max～0.25μm provide the best?t to the10μm silicate emission feature,based on a reducedχ2comparison with larger grain models. In comparison with other TWA members,this suggests lesser dust processing for2M1207, which could be explained by mechanisms such as aggregate fragmentation and/or turbulent mixing.We have obtained the best?t using an inner disk radius equal to the dust sublima-tion radius,indicating an absence of an inner disk hole.A?at disk of mass between10?4 and10?6M⊙,inclination between～60?and70?,and˙M of≤10?11M⊙yr?1provides a good ?t to2M1207disk.The disk mass estimate is a lower limit;longer wavelength observations can con?rm the presence of a population of much larger grains that dominate the disk mass but contribute little to the opacity at near-and mid-IR wavelengths.
We wish to thank the referee Barbara Whitney for many helpful comments and sug-gestions.Support for this work was provided by NASA Research Grant#NNG06GJ03G. Support for program9841was provided by NASA through a grant from STScI,which is operated by AURA Inc.,under NASA contract NAS5-26555.This work is based in part on observations made with the Spitzer Space Telescope,which is operated by the Jet Propulsion Laboratory,California Institute of Technology under a contract with NASA.Support for this work was provided by NASA through an award issued by JPL/Caltech.This work has made use of the SIMBAD database.
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Table1.IRAC and MIPS Observations a
I b J H K 3.6μm 4.5μm 5.8μm8μm24μm 3.8μm c8.7μm d10.4μmJy mJy mJy mJy mJy mJy mJy mJy mJy mJy mJy mJy
a Riaz et al.(2006).
b I and JHK magnitudes from DENIS and2MASS,respectively.
c Jayawardhana et.al.(2003).
d Sterzik et.al.(2004).
Table 2.Stellar and disk parameters
Parameter Value
-1.5
-1-0.5
00.5
11.5
-1-0.500.51 1.52 2.53 3.54
log F 24 (mJy)
l o g (F 24/F 4.5)
Fig.1.—Amount of ?aring in 2M1207disk.Dashed line represents a geometrically thin,op-tically thick ?at disk with a spectral slope λF λ∝λ?4/3.Solid line represents the photosphere of a brown dwarf at T eff =2600K.See text for more details.
-14-13.5
-13
-12.5
-12-11.5
-11-10.5-0.5 0 0.5 1
1.5 2
2.5
l o g ν F ν (e r g s /s /c m 2)log λ μm 1.251.171.151.11.051.0-14-13.5
-13
-12.5
-12-11.5
-11
-10.5
-0.5 0 0.5 1
1.5 2
2.5 3
l o g ν F ν (e r g s /s /c m 2)log λ μ
m -15-14.5
-14
-13.5
-13
-12.5-12
-11.5
-11
-10.5
l o g ν F ν (e r g s /s /c m 2)log λ μm Fig.2.—Top :(a)Variations in the SEDs with ?aring power β.Middle :(b)Models for disk masses ranging between 10?2M ⊙(top SED)and 10?9M ⊙(bottom SED).Bottom :(c)SEDs for 10viewing angles between edge-on (bottom SED)and face-on (top SED).Models for 63?and 69?(marked in black)provide the best ?t for 2M1207.The thin black dotted line in all ?gures represents the photospheric ?ux.
-14-13.5
-13
-12.5
-12-11.5
-11
-10.5-0.5 0 0.5 1
1.5 2
2.5
l o g ν F ν (e r g s /s /c m 2)log λ μm a max = 1 mm
a = 1 μm a max = 0.25 μm
-12.2-12
-11.8
-11.6-11.4
-11.2 0.7 0.8 0.9
1 1.1 1.2
l o g ν F ν (e r g s /s /c m 2)log λ μm a max = 1 mm
a = 1 μm a max = 0.25 μm
Fig. 3.—SEDs for three di?erent grain models:Blue -a max =1mm,red -a =1μm,black -a max =0.25μm.Top :(a)Variations in the SEDs are evident near 10μm and at far-IR/sub-mm wavelengths.Bottom :(b)The 10μm Si emission feature.Grain size of a max =0.25μm provides the best ?t.
-14-13.5
-13
-12.5
-12-11.5
-11-10.5
-1-0.5 0 0.5
1 1.5
2 2.5
l o g ν F ν (e r g s /s /c m 2)log λ μm -9-10-11-12-14-13.5
-13
-12.5
-12-11.5
-11-10.5
-0.5 0 0.5 1
1.5 2
2.5
l o g ν F ν (e r g s /s /c m 2)log λ μm stellar scattered inner rim disk rim+disk total -14-13.5
-13
-12.5
-12-11.5
-11-10.5
-0.5 0 0.5 1
1.5 2
2.5
l o g ν F ν (e r g s /s /c m 2)log λ μm 1 Rsub 3 Rsub 5 Rsub 7 Rsub Fig. 4.—Top :(a)
Variations in the SEDs with disk mass accretion rates between 10?9and 10?12M ⊙yr ?1.
Middle :(b)Separate contributions of the inner rim (wall)at the dust sublimation radius,
the disk,the stellar photosphere and the scattered ?ux.Bottom :(c)Models for di?erent inner disk radii.R in =1R sub provides the best ?t for 2M1207.
DELL 服务器硬盘掉线后的REBUILD修复操作全过程 注意：对阵列以及硬盘操作可能会导致数据丢失，请在做任何操作之前，确认您的数据已经妥善备份！！！ LSI BIOS界面下如何做硬盘修复 当硬盘配置阵列后，带有冗余的阵列，例如比较常用的RAID1与RAID5。在RAID 阵列使用中，如果因为某些原因（例如硬盘有坏道，硬盘检测不到，突然关机，断电等等）导致其中一块硬盘的数据未能及时更新，数据与其他硬盘无法同步，RAID卡就会把这块硬盘的状态标识为FAILED。根据RAID级别的算法特性，这样的阵列中允许有一块硬盘出现问题，系统仍然可以继续正常运行。 如果机器能够正常运行，而从外面可以看到一块硬盘闪黄灯，或者LCD上提示DRIVER FAILED，或者RAID卡报警，诸如此类的现象，说明这个时候阵列中有一块硬盘出现问题了。阵列虽然可以用，但是已经处于一个没有安全冗余的级别，要尽快修复！ 注意：发现有硬盘状态不正常时，请尽可能先将重要数据妥善备份！！！ 修复可以在系统下安装的Array Manager下进行，会有文档专门介绍，这里着重说明如何在LSI RAID BIOS中进行硬盘的修复。在硬盘修复中不需要用到的菜单功能将不着重介绍。 1、进入LSI RAID BIOS。在机器开机自检过程中按CTRL+M进入。 可以看到界面如下图： 2、为了保险起见，请先确认RAID级别，Objects-Logical Driver,选择要操作的逻辑驱动器，选择View/Update Parameters。
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尊重的素材（为人处世） 思路 人与人之间只有互相尊重才能友好相处 要让别人尊重自己，首先自己得尊重自己 尊重能减少人与人之间的摩擦 尊重需要理解和宽容 尊重也应坚持原则 尊重能促进社会成员之间的沟通 尊重别人的劳动成果 尊重能巩固友谊 尊重会使合作更愉快 和谐的社会需要彼此间的尊重 名言 施与人，但不要使对方有受施的感觉。帮助人，但给予对方最高的尊重。这是助人的艺术，也是仁爱的情操。—刘墉 卑己而尊人是不好的，尊己而卑人也是不好的。———徐特立 知道他自己尊严的人，他就完全不能尊重别人的尊严。———席勒 真正伟大的人是不压制人也不受人压制的。———纪伯伦 草木是靠着上天的雨露滋长的，但是它们也敢仰望穹苍。———莎士比亚 尊重别人，才能让人尊敬。———笛卡尔 谁自尊，谁就会得到尊重。———巴尔扎克 人应尊敬他自己，并应自视能配得上最高尚的东西。———黑格尔 对人不尊敬，首先就是对自己的不尊敬。———惠特曼
每当人们不尊重我们时，我们总被深深激怒。然而在内心深处，没有一个人十分尊重自己。———马克·吐温 忍辱偷生的人，绝不会受人尊重。———高乃依 敬人者，人恒敬之。———《孟子》 人必自敬，然后人敬之；人必自侮，然后人侮之。———扬雄 不知自爱反是自害。———郑善夫 仁者必敬人。———《荀子》 君子贵人而贱己，先人而后己。———《礼记》 尊严是人类灵魂中不可糟蹋的东西。———古斯曼 对一个人的尊重要达到他所希望的程度，那是困难的。———沃夫格纳 经典素材 1元和200元 （尊重劳动成果） 香港大富豪李嘉诚在下车时不慎将一元钱掉入车下，随即屈身去拾，旁边一服务生看到了，上前帮他拾起了一元钱。李嘉诚收起一元钱后，给了服务生200元酬金。 这里面其实包含了钱以外的价值观念。李嘉诚虽然巨富，但生活俭朴，从不挥霍浪费。他深知亿万资产，都是一元一元挣来的。钱币在他眼中已抽象为一种劳动，而劳动已成为他最重要的生存方式，他的所有财富，都是靠每天20小时以上的劳动堆积起来的。200元酬金，实际上是对劳动的尊重和报答，是不能用金钱衡量的。 富兰克林借书解怨 （尊重别人赢得朋友）
对翻译中异化法与归化法的正确认识 班级：外语学院、075班 学号：074050143 姓名：张学美 摘要：运用异化与归化翻译方法,不仅是为了让读者了解作品的内容,也能让读者通过阅读译作,了解另一种全新的文化,因为进行文化交流才是翻译的根本任务。从文化的角度考虑,采用异化法与归化法,不仅能使译文更加完美,更能使不懂外语的人们通过阅读译文,了解另一种文化,促进各民族人们之间的交流与理解。翻译不仅是语言符号的转换,更是跨文化的交流。有时,从语言的角度所作出的译文可能远不及从文化的角度所作出的译文完美。本文从翻译策略的角度，分别从不同时期来说明人们对异化法与归化法的认识和运用。 关键词:文学翻译；翻译策略；异化；归化；辩证统一 一直以来,无论是在我国还是在西方,直译(literal translation)与意译(liberal translation)是两种在实践中运用最多,也是被讨论研究最多的方法。1995年,美籍意大利学者劳伦斯-韦努蒂(Lawrence Venuti)提出了归化(domestication)与异化(foreignization)之说,将有关直译与意译的争辩转向了对于归化与异化的思考。归化与异化之争是直译与意译之争的延伸,是两对不能等同的概念。直译和意译主要集中于语言层面,而异化和归化则突破语言的范畴,将视野扩展到语言、文化、思维、美学等更多更广阔的领域。 一、归化翻译法 Lawrwnce Venuti对归化的定义是,遵守译入语语言文化和当前的主流价值观,对原文采用保守的同化手段,使其迎合本土的典律,出版潮流和政治潮流。采用归化方法就是尽可能不去打扰读者,而让作者向读者靠拢(the translator leaves the reader in peace, as much as possible, and moves the author towards him)。归化翻译法的目的在于向读者传递原作的基本精神和语义内容,不在于语言形式或个别细节的一一再现。它的优点在于其流利通顺的语言易为读者所接受,译文不会对读者造成理解上的障碍,其缺点则是译作往往仅停留在内容、情节或主要精神意旨方面,而无法进入沉淀在语言内核的文化本质深处。 有时归化翻译法的采用也是出于一种不得已,翻译活动不是在真空中进行的,它受源语文化和译语文化两种不同文化语境的制约,还要考虑到两种文化之间的
下面我说的是WIN7的服务.... Adaptive Brightness 监视氛围光传感器，以检测氛围光的变化并调节显示器的亮度。如果此服务停止或被禁用，显示器亮度将不根据照明条件进行调节。该服务的默认运行方式是手动，如果你没有使用触摸屏一类的智能调节屏幕亮度的设备，该功能就可以放心禁用。 Application Experience 在应用程序启动时为应用程序处理应用程序兼容性缓存请求。该服务的默认运行方式是自动，建议手动。 Application Information 使用辅助管理权限便于交互式应用程序的运行。如果停止此服务，用户将无法使用辅助管理权限启动应用程序，而执行所需用户任务可能需要这些权限。该服务的默认运行方式是手动，不建议更改。 Application Layer Gateway Service 为Internet 连接共享提供第三方协议插件的支持
如果装有第三方防火墙且不需要用ICS方式共享上网，完全可以禁用掉。 Application Management 为通过组策略部署的软件处理安装、删除以及枚举请求。如果该服务被禁用，则用户将不能安装、删除或枚举通过组策略部署的软件。如果此服务被禁用，则直接依赖于它的所有服务都将无法启动。该服务默认的运行方式为手动，该功能主要适用于大型企业环境下的集中管理，因此家庭用户可以放心禁用该服务。 Ati External Event Utility 装了ATI显卡驱动的就会有这个进程，建议手动。 Background Intelligent Transfer Service 使用空闲网络带宽在后台传送文件。如果该服务被禁用，则依赖于 BITS 的任何应用程序(如 Windows Update 或 MSN Explorer)将无法自动下载程序和其他信息。这个服务的主要用途还是用于进行WindowsUpdate或者自动更新，如果是采用更新包来更新的话，完全可以禁用。 Base Filtering Engine
几个最实用的硬盘修复解决方法 硬盘修复（1） 在研究硬盘故障的具体处理方法之前，我们有必要先了解一些硬盘相关的基础知识。 主引导记录区MBR 硬盘是一种磁介质的外部存储设备，在其盘片的每一面上，以转动轴为轴心、以一定的磁密度为间隔的若干同心圆就被划分成磁道（Track），每个磁道又被划分为若干个扇区（Sector），数据就按扇区存放在硬盘上。硬盘的第一个扇区（0道0头1扇区）被保留为主引导扇区。主引导扇区内主要有两项内容：主引导记录（对操作系统进行引导）和硬盘分区表。计算机启动时将读取该扇区的数据，并对其合法性进行判断（扇区最后两个字节是否为55AA或AA55），如合法则跳转执行该扇区的第一条指令。所以硬盘的主引导区常常成为病毒攻击的对象，从而被篡改甚至被破坏。硬盘控制器 硬盘控制器是硬盘及其他具有相同接口规范的外部设备（如CD-ROM驱动器）的管理者，由它来完成驱动器与内存之间的命令及数据传输。硬盘控制器发生故障或连接不正确将会导致硬盘无法正常工作。 CMOS中的硬盘信息 在计算机的CMOS中也存储了硬盘的信息，主要有硬盘类型、容量、柱面数、磁头数、每道扇区数、寻址方式等内容，对硬盘参数加以说明，以便计算机正确访问硬盘。 当CMOS因故掉电或发生错误时（启动时一般会提示“CMOS Checksum Error”或类似信息），硬盘设置可能会丢失或错误，硬盘访问也就无法正确进行。这种情况我们就必须重新设置硬盘参数，如果事先已记下硬盘参数或者有某些防病毒软件事先备份的CMOS信息，只需手工恢复即可；否则也可使用BIOS设置（Setup）中的“自动检测硬盘型”（HD Type Auto Detection）的功能，一般也能得到正确的结果。 不是问题的问题 很多时候我们的电脑会出现一些看似不得了的毛病，其实只是自己吓自己，也就是拨拨线头、动动跳线的举手之劳。常见的让你空出一身冷汗的硬盘不自举问题主要有以下两种： 系统不承认硬盘： 此类故障最为常见，开机自检完成时提示以下出错信息： HDD controller failure Press F1 to Resume 上述E文意指“硬盘无法启动”，甚至有时用CMOS中的自动监测功能也无法发现硬盘的存在。当出现上述信息时，应该重点先检查与硬盘有关的电源线、数据线的接口有无损坏、松动、接触不良、反接等现象，此外常见的原因就是硬盘上的主从跳线是否设置错误。 检查、排除方法： 重新插拔硬盘电源线、数据线或者将数据线改插其他IDE口进行替换试验。
开机老出现硬盘修复解决方法 开机老出现硬盘修复 解决方法如下 ①单击“开始→运行”，在“运行”对话框中输入“regedit”打开注册表编辑器，依次选择 HKEY_LOCAL_MACHINE\SYSTEM\CurrentControlSet\Control\Session Manager 右边找到BootExecute，将其数值全部清空 这样计算机永远就不会在启动的时候检测硬盘了 ②以管理员身份登录WinXP后，在命令提示符窗口中输入“chkntfs /x [盘符]”即可，例如要屏蔽扫描C 盘，则输入“chkntfs /x C：”（不含引号）
③在运行中输入msconfig 在启动项中把碎片整理程序前面的小勾去掉. 【注】系统关闭开机磁盘扫描chkntfs与chkdsk Microsoft 已经开发了 Chkntfs.exe 实用工具，该实用工具可以在 Microsoft Windows NT 4.0 Service Pack 2 及更新版本的 Windows 中找到。该实用工具被设计为：当 Windows 在非正常关机后重新启动时，禁止在特定卷上自动运行 chkdsk。如果使用 chkdsk /f 安排了在下一次系统重新启动时在活动卷上运行 chkdsk，则也可以使用 chkntfs 来取消安排 chkdsk。 chkntfs drive: [...] chkntfs /d chkntfs /x drive: [...] chkntfs /c drive: [...]
drive:指定驱动器号。 /D 将计算机还原为默认状态，启动时检查所有驱动器并对有问题的驱动器执行chkdsk 命令。这将取消 /X 选项的效果。 /X 排除默认启动时检查的驱动器。上次执行此命令排除的驱动器此时无效。 /C 如果已经设置了非正常位，则安排在下一次重新启动时运行 chkdsk。 示例： chkntfs /x c: 此命令禁止 chkdsk 在驱动器 C: 上运行 chkntfs /x d:e:此命令禁止 chkdsk 在驱动器 D: 和 E: 上运行 chkntfs /x 命令不是累积性的，该命令会覆盖以前建立的任何驱动器排除项。在上面的示例中，chkntfs 命令只禁止 chkdsk 在驱动器 D 和 E 上进行检查，不检查驱动器 C 是否存在非正常位。
“异化”与“归化”之间的关系并评述 1、什么是归化与异化 归化”与“异化”是翻译中常面临的两种选择。钱锺书相应地称这两种情形叫“汉化”与“欧化”。A．归化 所谓“归化”（domestication 或target-language-orientedness），是指在翻译过程中尽可能用本民族的方式去表现外来的作品；归化翻译法旨在尽量减少译文中的异国情调，为目的语读者提供一种自然流畅的译文。Venuti 认为，归化法源于这一著名翻译论说，“尽量不干扰读者，请作者向读者靠近” 归化翻译法通常包含以下几个步骤：（1）谨慎地选择适合于归化翻译的文本；（2）有意识地采取一种自然流畅的目的语文体；（3）把译文调整成目的语篇体裁；（4）插入解释性资料；（5）删去原文中的实观材料；（6）调协译文和原文中的观念与特征。 B．“异化”（foreignization或source-language-orientedness）则相反，认为既然是翻译，就得译出外国的味儿。异化是根据既定的语法规则按字面意思将和源语文化紧密相连的短语或句子译成目标语。例如，将“九牛二虎之力”译为“the strength of nine bulls and two tigers”。异化能够很好地保留和传递原文的文化内涵，使译文具有异国情调，有利于各国文化的交流。但对于不熟悉源语及其文化的读者来说，存在一定的理解困难。随着各国文化交流愈来愈紧密，原先对于目标语读者很陌生的词句也会变得越来越普遍，即异化的程度会逐步降低。 Rome was not built in a day. 归化:冰冻三尺,非一日之寒. 异化:罗马不是一天建成的. 冰冻三尺,非一日之寒 异化:Rome was not built in a day. 归化:the thick ice is not formed in a day. 2、归化异化与直译意译 归化和异化，一个要求“接近读者”，一个要求“接近作者”，具有较强的界定性；相比之下，直译和意译则比较偏重“形式”上的自由与不自由。有的文中把归化等同于意译，异化等同于直译，这样做其实不够科学。归化和异化其实是在忠实地传达原作“说了什么”的基础之上，对是否尽可能展示原作是“怎么说”，是否最大限度地再现原作在语言文化上的特有风味上采取的不同态度。两对术语相比，归化和异化更多地是有关文化的问题，即是否要保持原作洋味的问题。 3、不同层面上的归化与异化 1、句式 翻译中“归化”表现在把原文的句式（syntactical structure）按照中文的习惯句式译出。
电脑不认硬盘的处理办法 故障现象一：开机后屏幕显示："Device error"，然后又显示："Non-System disk or disk er ror，Replace and strike any key when ready"，说明硬盘不能启动。用软盘启动后，在A：＞后键人C：，屏幕显示："Invalid drive specification"，系统不认硬盘。 故障分析及处理：造成该故障的原因一般是CMOS中的硬盘设置参数丢失或硬盘类型设置错误造成的。进入CMOS，检查硬盘设置参数是否丢失或硬盘类型设置是否错误。如果确是该种故障，只需将硬盘设置参数恢复或修改过来即可。如果不会修改硬盘参数，也可用备份过的CMOS信息进行恢复，如果你没有备份CMOS信息，也别急，有些高档微机的CM OS设置中有"HDD AUTO DETECTION"(硬盘自动检测)选项，可自动检测出硬盘类型参数。若无此项，只好打开机箱，查看硬盘表面标签上的硬盘参数，照此修改即可。 故障现象二：开机后，"WAIT"提示停留很长时间，最后出现"HDD controller Failure"。 故障分析及处理：造成该故障的原因一般是硬盘线接口接触不良或接线错误。先检查硬盘电源线与硬盘的连接，再检查硬盘数据信号线与多功能卡或硬盘的连接，如果连接松动或连线接反都会有上述提示，最好是能找一台型号相同且使用正常的微机，可以对比线缆的连接。 故障现象三：开机后，屏幕上显示："Invalid partition table"，硬盘不能启动。 故障分析及处理：造成该故障的原因一般是硬盘主引导记录中的分区表有错误，当指定了多个自举分区(只能有一个自举分区)或病毒(一种具有隐蔽性破坏性传染性的恶意代码)占用了分区表时，将有上述提示。主引导记录(MBR)位于0磁头/0柱面/1扇区，由FDISK.EXE 对硬盘分区时生成。MBR包括主引导程序、分区表和结束标?quot;55AAH"三分，共占一个扇区。主引导程序中含有检查硬盘分区表的程序代码和出错信息、出错处理等内容。当硬盘启动时，主引导程序将检查分区表中的自举标志。若某个分区为可自举分区，则有分区标志8OH，否则为00H，系统规定只能有一个分区为自举分区，若分区表中含有多个自举标志时，主引导程序会给出"Invalid partion table"的错误提示。最简单的解决方法是用NDD修复，它将检查分区表中的错误。若发现错误，将会询问你是否愿意修改，你只要不断地回答YE S即可修正错误，或者用备份过的分区表覆盖它也行(KV300，NU8.O中的RESCUE都具有备份与恢复分区表的功能)。如果是病毒(一种具有隐蔽性破坏性传染性的恶意代码)感染了分区表，格式化是解决不了问题的，可先用杀毒软件(反病毒软件或防毒软件是用于消除电脑病毒特洛伊木马和恶意软件的一类软件)杀毒，再用NDD进行修复。如果上述方法都不能解决，还有一招。就是先用FDISK重新分区，但分区大小必须和原来的分区一样，这一点尤为重要，分区后不要进行高级格式化，然后用NDD进行修复。修复后的硬盘不但能启动，而且硬盘上的信息也不会丢失。其实用FDISK分区，相当于用正确的分区表覆盖原来的分区表。尤其当用软盘启动后不认硬盘时，这一招特灵。 故障现象四：开机后自检完毕，从硬盘启动时死机或者屏幕上显示："No ROM Basic，Sys tem Halted"。
谈如何尊重人尊重他人，我们赢得友谊；尊重他人，我们收获真诚；尊重他人，我们自己也 获得尊重；相互尊重，我们的社会才会更加和谐. ——题记 尊重是对他人的肯定，是对对方的友好与宽容。它是友谊的润滑剂，它是和谐的调节器， 它是我们须臾不可脱离的清新空气。“主席敬酒，岂敢岂敢？”“尊老敬贤，应该应该！”共和 国领袖对自己老师虚怀若谷，这是尊重；面对许光平女士，共和国总理大方的叫了一 声“婶婶”，这种和蔼可亲也是尊重。 尊重不仅会让人心情愉悦呼吸平顺，还可以改变陌生或尖锐的关系，廉颇和蔺相如便是 如此。将相和故事千古流芳:廉颇对蔺相如不满，处处使难，但蔺相如心怀大局，对廉颇相 当的尊重，最后也赢得了廉颇的真诚心，两人结为好友，共辅赵王，令强秦拿赵国一点办法 也没有。蔺相如与廉颇的互相尊重，令得将相和的故事千百年令无数后人膜拜。 现在，给大家举几个例子。在美国，一个颇有名望的富商在散步 时，遇到一个瘦弱的摆地摊卖旧书的年轻人，他缩着身子在寒风中啃着发霉的面包。富 商怜悯地将8美元塞到年轻人手中，头也不回地走了。没走多远，富商忽又返回，从地摊上 捡了两本旧书，并说：“对不起，我忘了取书。其实，您和我一样也是商人！”两年后，富商 应邀参加一个慈善募捐会时，一位年轻书商紧握着他的手，感激地说：“我一直以为我这一生 只有摆摊乞讨的命运，直到你亲口对我说，我和你一样都是商人，这才使我树立了自尊和自 信，从而创造了今天的业绩??”不难想像，没有那一 句尊重鼓励的话，这位富商当初即使给年轻人再多钱，年轻人也断不会出现人生的巨变， 这就是尊重的力量啊 可见尊重的量是多吗大。大家是不是觉得一个故事不精彩，不够明确尊重的力量，那再 来看下一个故事吧！ 一家国际知名的大企业，在中国进行招聘，招聘的职位是该公司在中国的首席代表。经 过了异常激烈的竞争后，有五名年轻人，从几千名应聘者中脱颖而出。最后的胜出者，将是 这五个人中的一位。最后的考试是一场面试，考官们都 作文话题素材之为人处世篇：尊重 思路 人与人之间只有互相尊重才能友好相处 要让别人尊重自己，首先自己得尊重自己 尊重能减少人与人之间的摩擦 尊重需要理解和宽容 尊重也应坚持原则 尊重能促进社会成员之间的沟通 尊重别人的劳动成果 尊重能巩固友谊 尊重会使合作更愉快 和谐的社会需要彼此间的尊重 名言 施与人，但不要使对方有受施的感觉。帮助人，但给予对方最高的尊重。这是助人的艺 术，也是仁爱的情操。———刘墉 卑己而尊人是不好的，尊己而卑人也是不好的。———徐特立 知道他自己尊严的人，他就完全不能尊重别人的尊严。———席勒 真正伟大的人是不压制人也不受人压制的。———纪伯伦 草木是靠着上天的雨露滋长的，但是它们也敢仰望穹苍。———莎士比亚
万方数据
万方数据
万方数据
万方数据
翻译的归化与异化 作者：熊启煦 作者单位：西南民族大学,四川,成都,610041 刊名： 西南民族大学学报（人文社科版） 英文刊名：JOURNAL OF SOUTHWEST UNIVERSITY FOR NATIONALITIES（HUMANITIES AND SOCIAL SCIENCE） 年，卷(期)：2005,26(8) 被引用次数：14次 参考文献(3条) 1.鲁迅且介亭杂文二集·题未定草 2.刘英凯归化--翻译的歧路 3.钱钟书林纾的翻译 引证文献(15条) 1.郭锋一小议英语翻译当中的信达雅[期刊论文]-青春岁月 2011(4) 2.许丽红论汉英语言中的文化差异与翻译策略[期刊论文]-考试周刊 2010(7) 3.王笑东浅谈汉英语言中的差异与翻译方法[期刊论文]-中国校外教育（理论） 2010(6) 4.王宁中西语言中的文化差异与翻译[期刊论文]-中国科技纵横 2010(12) 5.鲍勤.陈利平英语隐喻类型及翻译策略[期刊论文]-云南农业大学学报(社会科学版) 2010(2) 6.罗琴.宋海林浅谈汉英语言中的文化差异及翻译策略[期刊论文]-内江师范学院学报 2010(z2) 7.白蓝跨文化视野下文学作品的英译策略[期刊论文]-湖南社会科学 2009(5) 8.王梦颖探析汉英语言中的文化差异与翻译策略[期刊论文]-中国校外教育（理论） 2009(8) 9.常晖英汉成语跨文化翻译策略[期刊论文]-河北理工大学学报（社会科学版） 2009(1) 10.常晖对翻译文化建构的几点思考[期刊论文]-牡丹江师范学院学报（哲学社会科学版） 2009(4) 11.常晖认知——功能视角下隐喻的汉译策略[期刊论文]-外语与外语教学 2008(11) 12.赵勇刚汉英语言中的文化差异与翻译策略[期刊论文]-时代文学 2008(6) 13.常晖.胡渝镛从文化角度看文学作品的翻译[期刊论文]-重庆工学院学报(社会科学版) 2008(7) 14.曾凤英从文化认知的视角谈英语隐喻的翻译[期刊论文]-各界 2007(6) 15.罗琴.宋海林浅谈汉英语言中的文化差异及翻译策略[期刊论文]-内江师范学院学报 2010(z2) 本文链接：https://www.doczj.com/doc/fe15727025.html,/Periodical_xnmzxyxb-zxshkxb200508090.aspx
手工修正结构需要一定的数据恢复基础原理知识。在这里我们只描述常用几种系统结构位的手工修正，包括DBR、FAT表头部、MFT头部。 欢迎阅读本文，这是我们的《走进科学--探索发现--硬盘分区信息丢失之谜》的第三篇《W inHex应用之奇怪的未格式化》这篇文章是三篇文章中最绕的一篇，充分认识硬盘数据结构的“C T”运行 WINHEX之后你会觉得，这个可以学，很好很强大。在第一篇《寻找丢失的硬盘分区》文章里，我们恢复了客户故障硬盘的分区信息，但仍然有三个分区是未格式化状态，在这篇文章中我们利用非常强大的Winhex来进行手工修复文件系统。第二篇《DiskGenius恢复提示格式化的数据》中使用硬盘数据恢复软件的新星DiskGenius恢复这三个分区的数据，使用的是扫描重组目录法，直接提取数据。 前面恢复的6个分区中，有3个48.8G的NTFS分区是提示“未格式化”的，我们在前面介绍的是使用磁盘精灵直接扫描恢复数据，除扫描方法恢复数据，我们还可以使用WINHEX磁盘编辑工具直接修改异常扇区，达到恢复数据的目的。除了恢复结果原汁原味，而且恢复迅速，熟练后只需几分钟恢复这三个异常分区。
运行WINHEX，点取打开磁盘，选择我们要编辑恢复的硬盘，然后确定打开,这里选择物理驱动器，有的时候如果单一分区文件系统有问题，打开逻辑驱动器会出现问题，最好是打开物理驱动器后在对单一分区进行操作。
打开物理驱动器后，6个分区信息一目了然，其中2、3、4分区格式位置是未知的文件系统，显示？号，看来这三个分区引导信息扇区DBR肯定出问题了。
点击分区1，扇区内容栏将跳到分区1开始的地方，也就是分区的DBR位置。我们看到分区1从63扇区开始，其DBR的开始字节为EB 58 90
翻译作业10 Nov 15 一、请按归化法(Domestication)翻译下列习语。 Kill two birds with one stone a wolf in sheep’s clothing strike while the iron is hot. go through fire and water add fuel to the flames / pour oil on the flames spring up like mushrooms every dog has his day keep one’s head above water live a dog’s life as poor as a church mouse a lucky dog an ass in a lion’s skin a wolf in sheep’s clothing Love me, love my dog. a lion in the way lick one’s boots as timid as a hare at a stone’s throw as stupid as a goose wet like a drown rat as dumb as an oyster lead a dog’s life talk horse One boy is a boy, two boys half a boy, and three boys nobody. Man proposes, God disposes. Cry up wine and sell vinegar (cry up, to praise; extol: to cry up one's profession) Once bitten, twice shy. An hour in the morning is worth two in the evening． New booms sweep clean. take French leave seek a hare in a hen’s nest have an old head on young shoulder Justice has long arms You can’t teach an old dog Rome was not built in a day. He that lives with cripples learns to limp. Everybody’s business is nobody’s business. The more you get, the more you want. 二、请按异化法(foreignization)翻译下列习语。 Kill two birds with one stone a wolf in sheep’s clothing
无需任何软件，简单修改Win7开机登陆界面背景图片，让您的电脑更为个性。 默认分类2010-09-27 15:48:45 阅读134 评论0 字号：大中小订阅 无需任何软件，自定义Win7开机登陆界面背景图片，让您的电脑更为个性。 Win7已经出来很长时间，其实类似修改Win7开机登陆界面举不胜举，比如ThoosjeLogonEditor等。但是用软件到底都修改了系统的什么文件？系统文件吗？会不会造成系统不稳定啊？ 最近找到了这样一个方法，利用微软提供给各大厂商制作OEM版Win7时定制登陆界面的方法，自定义Win7开机登陆界面背景图片，方法很简单，也很实际，不修改任何文件，只要修改一下一个注册表键值，添加一张图片，即可。 以下操作请以管理员权限进行。 1.准备图片：将需要作为背景图片的图片格式转换成.jpg，文件大小控制在250KB以内（否则可能无法正常显示），图片分辨率调整成当前显示器分辨率，将图片命名为“backgroundDefault.jpg” 2.打开注册表编辑器regedit：可以“开始”→“运行”→键入“regedit”→“确定”→启动注册表编辑器。 3.展开到： [HKEY_LOCAL_MACHINE\SOFTWARE\Microsoft\Windows\CurrentVersion\Authentication\LogonUI\Ba ckground]→右侧新建一个双字节值“OEMBackground”（OEM版本的Win7已经有这个键值）→右击该双字节值→“修改”→将键值修改为“1”。 图：
无需任何软件，简单修改Win7开机登陆界面背景图片，让您的电脑更为个性。 4.分两种情况 A:普通用户（相对于OEM用户，登陆界面是Win7标准的，而不是OEM定制的） “我的电脑”→“C:\Windows\System32\oobe”→在该目录下创建一个名为“info”的文件夹并打开→在打开的目录下创建一个名为“backgrounds”的文件夹→将准备好的“backgroundDefault.jpg”复制到这个位置（即C:\Windows\System32\oobe\info\Backgrounds）。 B:OEM用户（登陆界面已由OEM定制） “我的电脑”→“C:\Windows\System32\oobe\info\Backgrounds”，用准备好的“backgroundDefault.jpg”覆盖已存在的文件（可以先把已存在的文件备份，随你喜欢）
电脑硬盘岀现坏道的检测和修复 电脑硬盘使用过久就会出现各种各样的问题，比如硬盘的操 作速度相比以前变得很慢，并且长时间反复读盘，然后出错，或windows提示“无法读取或无法写入文件”，严重时出现蓝屏等现象。这些都是由于出现坏道而引起的。硬盘坏道是由于硬盘除了本身质量以及老化的原因外，也有一部分是由于平时使用不当造成的。硬盘坏道分为逻辑坏道和物理坏道两种，前者为软坏道，通常为软件操作或使用不当造成的，可用软件修复；后者为真正的物理性坏道，它表明你的硬盘磁道上产生了物理损伤，只能通过更改硬盘分区或扇区的使用情况来解决。 如何检测自己的硬盘是否有坏道 由于之前检测硬盘坏道方法多数用的是在纯dos下的软盘检测，而现在优盘代替软盘，所以软驱也从电脑中消失。下面笔者介绍的是ghostxp安装盘自带的效率源大容量硬盘检测修复程序。 将电脑设置成光盘启动项，然后会出现选择界面，选择［9］硬盘内存检测维修工具，单击回车。 单击效率源硬盘检测修复程序，进去程序界面。 这个界面我们主要应用的便是“硬盘全面检测”选项，当扫 描到坏到时候，会在右面的“已知坏磁道信息”中显示出来。其中的“硬盘高级检测”选项是可以自定义起始位置和结束位置，但对
于大多数用户来说还是选择第一项比较妥当。 如何修复已知的硬盘坏道 当得知自己硬盘出现坏道的时候，千万别慌张，首先应该确 认硬盘的坏道是逻辑坏道还是物理坏道，其方法比较简单，仍然是使用刚刚的ghost光盘启动，然后运行[3]dos增强版及工具集，执行“scandisk”，scandisk程序便会检查硬盘，对产生的逻辑坏道会自行弹出对话框，选择“fixit”对逻辑坏道进行初级修复。如扫描程序在某一进度停滞不前，那么硬盘就有了物理坏道。 当检测是逻辑坏道时，我们可以尝试用windows自带的工 具。进入“我的电脑”中选择有逻辑坏道的硬盘，单击鼠标右键，选择“属性” 一“工具”?“开始检查”就弹出“磁盘扫描程序”,选中“完全”并将“自动修复错误”打上勾，单击“开始”，就开始对该分区进行扫描和修复。 对于物理坏道来说就有些麻烦，如果再保的硬盘可以找商家 解决，但是如果过保的硬盘就只能自行解决。最常见的解决方法是用分区工具，如分区魔术师、xp安装版自带的分区工具等，通过对硬盘的重新分区，隐藏有物理坏道的硬盘空间，对其实行隔离。 当然，有时候不管怎么隔离都会检测出坏道出现，这时候的 办法就只有进行低级格式化。要知道低级格式化是万不得已的方法，所以笔者建议用户慎用。因为低格是将空白的磁盘重新划分出柱面和磁道和扇区、标准地址等信息，会对硬盘造成剧烈磨损。 低级格式化只能在dos环境下完成，运行lformat命令后就可
尊重他人的写作素材 导读：——学生最需要礼貌 著名数学家陈景润回厦门大学参加 60 周年校庆，向欢迎的人们说的第一句话是：“我非常高兴回到母校，我常常怀念老师。”被人誉为“懂得人的价值”的著名经济学家、厦门大学老校长王亚南，曾经给予陈景润无微不至的关心和帮助。陈景润重返母校，首先拜访这位老校长。校庆的第三天，陈景润又出现在向“哥德巴赫猜想”进军的启蒙老师李文清教授家中，陈景润非常尊重和感激他。他还把最新发表的数学论文敬送李教授审阅，并在论文扉页上工工整整写了以下的字：“非常感谢老师的长期指导和培养——您的学生陈景润。”陈景润还拜访了方德植教授，方教授望着成就斐然而有礼貌的学生，心里暖暖的。 ——最需要尊重的人是老师 周恩来少年时在沈阳东关模范学校读书期间 , 受到进步教师高盘之的较大影响。他常用的笔名“翔宇”就是高先生为他取的。周恩来参加革命后不忘师恩 , 曾在延安答外国记者问时说：“少年时代我在沈阳读书 , 得山东高盘之先生教诲与鼓励 , 对我是个很大的 促进。” 停奏抗议的反思 ——没有礼仪就没有尊重 孔祥东是著名的钢琴演奏家。 1998 年 6 月 6 日晚，他在汕头
举办个人钢琴独奏音乐会。演出之前，节目主持人再三强调，场内观众不要随意走动，关掉 BP 机、手提电话。然而，演出的过程中，这种令人遗憾的场面却屡屡发生：场内观众随意走动， BP 机、手提电话响声不绝，致使孔祥东情绪大受干扰。这种情况，在演奏舒曼作品时更甚。孔祥东只好停止演奏，静等剧场安静。然而，观众还误以为孔祥东是在渴望掌声，便报以雷鸣般的掌声。这件事，令孔祥东啼笑皆非。演出结束后，孔祥东说：有个 BP 机至少响了 8 次，观众在第一排来回走动，所以他只得以停奏抗议。 “礼遇”的动力 ——尊重可以让人奋发 日本的东芝公司是一家著名的大型企业，创业已经有 90 多年的历史，拥有员工 8 万多人。不过，东芝公司也曾一度陷入困境，土光敏夫就是在这个时候出任董事长的。他决心振兴企业，而秘密武器之一就是“礼遇”部属。身为偌大一个公司的董事长，他毫无架子，经常不带秘书，一个人步行到工厂车间与工人聊天，听取他们的意见。更妙的是，他常常提着酒瓶去慰劳职工，与他们共饮。对此，员工们开始都感到很吃惊，不知所措。渐渐地，员工们都愿意和他亲近，他赢得了公司上下的好评。他们认为，土光董事长和蔼可亲，有人情味，我们更应该努力，竭力效忠。因此，土光上任不久，公司的效益就大力提高，两年内就把亏损严重、日暮途穷的公司重新支撑起来，使东芝成为日本最优秀的公司之一。可见，礼，不仅是调节领导层之间关
尊重_议论文素材 "礼遇"的动力 --尊重可以让人奋发 日本的东芝公司是一家著名的大型企业，创业已经有90 多年的历史，拥有员工8 万多人。不过，东芝公司也曾一度陷入困境，土光敏夫就是在这个时候出任董事长的。他决心振兴企业，而秘密武器之一就是"礼遇"部属。身为偌大一个公司的董事长，他毫无架子，经常不带秘书，一个人步行到工厂车间与工人聊天，听取他们的意见。更妙的是，他常常提着酒瓶去慰劳职工，与他们共饮。对此，员工们开始都感到很吃惊，不知所措。渐渐地，员工们都愿意和他亲近，他赢得了公司上下的好评。他们认为，土光董事长和蔼可亲，有人情味，我们更应该努力，竭力效忠。因此，土光上任不久，公司的效益就大力提高，两年内就把亏损严重、日暮途穷的公司重新支撑起来，使东芝成为日本最优秀的公司之一。可见，礼，不仅是调节领导层之间关系的纽带，也是调节上下级之间关系，甚至和一线工人之间关系的纽带。世界知识产权日 --尊重知识 在2000 年10 月召开的世界知识产权组织第35 届成员国大会上，我国提议将 4 月26 日定为"世界知识产权日"。这个提案经世界知识产权组织成员国大会得到了确定。2001 年4 月26 日成为第一个"世界知识产权日"。这是我国尊重知识的具体表现。 屠格涅夫与乞丐 --尊重比金钱更重要 俄罗斯文豪屠格涅夫一日在镇上散步，路边有一个乞丐伸手向他讨钱。他很想有所施与，从口袋掏钱时才知道没有带钱袋。见乞丐的手伸得高高地等着，屠格涅夫面有愧色，只好握着乞丐的手说："对不起，我忘了带钱出来。"乞丐笑了，含泪说："不，我宁愿接受您的握手。" 孙中山尊重护士 --尊重不分社会地位 有一天，孙中山先生病了，住院治疗。当时，孙中山已是大总统、大元帅了。但是，他对医务人员很尊重，对他们讲话很谦逊。平时，无论是早晨或是晚间，每当接到护士送来的药品，他总是微笑着说声"谢谢您"，敬诚之意溢于言辞。 1925 年孙中山患肝癌，弥留之际，当一位护理人员为他搬掉炕桌时，孙中山先生安详地望着她，慈祥地说："谢谢您，您的工作太辛苦了，过后您应该好好休息休息，这阵子您太辛苦了! "听了这话，在场的人都泣不成声。 毛泽东敬酒 --敬老尊贤是一种美德 1959 年6 月25 日，毛泽东回到离别30 多年的故乡韶山后，请韶山老人毛禹珠来吃饭，并特地向他敬酒。毛禹珠老人说："主席敬酒，岂敢岂敢! "毛泽东接着说："敬老尊贤，应该应该。" 周恩来不穿拖鞋接待外宾 --衣着整齐体现对人的尊重 周恩来晚年病得很重，由于工作的需要，他还要经常接待外宾。后来，他病得连脚都肿起来了，原先的皮鞋、布鞋都不能穿，他只能穿着拖鞋走路，可是，有些重要的外事活动，他还是坚持参加。他身边的工作人员出于对总理的爱护和关心，对他说："您就穿着拖鞋接待外
关于尊重的论点和论据素材 关于尊重的论点 1.尊重需要理解和宽容。 2.尊重也应该坚持原则。 3.尊重知识是社会进步的表现。 4.尊重别人就要尊重别人的劳动。 5.尊重人才是社会发展的需要。 6.人与人之间需要相互尊重。 7.只有尊重别人才会受到别人的尊重。 8.尊重能促进人与人之间的沟通。 9.我们应该养成尊重他人的习惯。 10.对人尊重，常会产生意想不到的善果。 关于尊重的名言 1.仁者必敬人。《荀子》 2.忍辱偷生的人决不会受人尊重。高乃依 3.尊重别人的人不应该谈自己。高尔基 4.尊重别人，才能让人尊敬。笛卡尔 5.谁自尊，谁就会得到尊重。巴尔扎克 6.君子贵人而贱己，先人而后己。《礼记》 7.卑己而尊人是不好的，尊己而卑人也是不好的。徐特立 8.对人不尊敬，首先就是对自己的不尊敬。惠特曼
9.为人粗鲁意味着忘记了自己的尊严。车尔尼雪夫斯基 10.对人不尊敬的人，首先就是对自己不尊重。陀思妥耶夫斯基 11.对于应尊重的事物，我们应当或是缄默不语，或是大加称颂。尼采 12.尊重老师是我们中华民族的传统美德，我们每一个人都不应该忘记。xx 13.尊重劳动、尊重知识、尊重人才、尊重创造。《xx 大报告》 14.对别人的意见要表示尊重。千万别说：你错了。卡耐基 15.尊重人才，培养人才，是通用电器长久不败的法宝。杰克韦尔奇 16.君子之于人也，当于有过中求无过，不当于无过中求有过。程颐 17.施与人，但不要使对方有受施的感觉。帮助人，但给予对方最高的尊重。这是助人的艺术，也是仁爱的情操。刘墉 18.要尊重每一个人，不论他是何等的卑微与可笑。要记住活在每个人身上的是和你我相同的性灵。叔本华 19.要喜欢我们所不尊重的人是很难的;但要喜欢
硬盘起死回生术-高手告诉您修复硬盘的办法
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（1）在读取某一文件或运行某一程序时，硬盘反复读盘且出错，提示文件损坏等信息，或者要经过很长时间才能成功；有时甚至会出现蓝屏等； （2）硬盘声音突然由原来正常的摩擦音变成了怪音； （3）在排除病毒感染的情况下系统无法正常启动，出现“Sector not found”或“General error in reading drive C”等提示信息； （4）Format硬盘时，到某一进度停止不前，最后报错，无法完成；
（5）每次系统开机都会自动运行Scandisk扫描磁盘错误； （6）对硬盘执行FDISK时，到某一进度会反复进进退退； （7）启动时不能通过硬盘引导系统，用软盘启动后可以转到硬盘盘符，但无法进入，用SYS命令传导系统也不能成功。这种情况很有可能是硬盘的引导扇区出了问题。 常识：坏道修复方法- 具体问题具体分析
由于硬盘内部工作环境的要求极为严格，小小的灰尘进入到硬盘内部也会造成不可挽回的损坏，所以当硬盘出现坏道时，我们并不能拆开硬盘进行维修，只能够通过一些工具软件来进行修复，从而最大限度的挽回损失。 一般情况下，硬盘产生逻辑坏道的原因是一些正版软件会在硬盘上某些扇区写入信息，其他的软件则无法访问这个扇区，这种情况下，硬盘检测工具也会误认为该扇区产生了坏道，一般这种情况无需进行修复，但是现在的软件越来越少的采用这种加密方式了。 还有一种情况就是使用不当造成的了，例如硬盘在读取数据时意外遭到重启，则有可能产生逻辑坏道，情况严重的甚至会产生物理坏道。我们此时可以使用Windows自带的磁盘工具对硬盘进行扫描，并且对错误进行自动修复。