Consistency of the metallicity distributions of nearby F, G and K dwarfs

a r X i v :a s t r o -p h /9808335v 1 28 A u g 1998

A&A manuscript no.

(will be inserted by hand later)

ASTRONOMY

AND

ASTROPHY SICS

1.Introduction

Thirty six years after its discovery by van den Bergh (1962),the G dwarf problem still presents challenges to the astrophysicists studying Galactic Evolution.Although several mechanisms for decreasing the number of metal-poor dwarfs in the Galaxy have already been devised,the shape of the metallicity distribution is generally not very well reproduced by the majority of models in the liter-ature.In fact,given the uncertainties in the data,ob-taining a good ?t to the G dwarf metallicity distribu-tion was less signi?cant than to search for an explanation for the paucity of metal-poor objects.However,after the recent derivation of a new G dwarf metallicity distribu-tion (Rocha-Pinto &Maciel 1996,hereafter RPM),the G dwarf problem cannot be regarded as just the paucity of metal-poor stars,compared with Simple Model pre-

2H.J.Rocha-Pinto&W.J.Maciel:Consistent metallicity distributions amongst F,G and K dwarfs dwarf metallicity distribution,and the consistency of the

metallicity distributions of late-type dwarfs of types F,G,

and K is considered.In Sect.4,we present the proposed

corrections owing to the chromospheric activity,and apply

them to both G and K dwarf metallicity distributions.A

discussion of the results by Favata et al.(1997),especially

regarding the di?erences between their derived distribu-

tions is given in Sect.5.

2.The K dwarf metallicity distribution

We have selected a preliminary sample from the Third

Catalogue of Nearby Stars(Gliese&Jahrei?1991;here-

after CNS3).This sample comprises around870objects

classi?ed as K stars.We searched for uvby indices for these stars in the surveys of Olsen(1993,1994)and in the com-pilation by Hauck&Mermilliod(1998),favouring the data by Olsen when a star had measurements in both sources. Disregarding unresolved binaries,stars with variable in-dices,giants and subgiants,our sample has been reduced to242objects.For some of these,the spectral types avail-able in the literature do not allow the identi?cation of the star luminosity class.In these cases,the identi?cation was made by checking the star’s position on the(b?y)×c1 diagram.Seventeen objects occupy a region in this dia-gram which is mainly populated by subgiants,according to Olsen(1984),and were eliminated from the sample. One star(BD+003077)was also removed from the sam-ple,as it has a colour(b?y)=0.972of an M dwarf, although being classi?ed as K7V in the CNS3.

Metallicities were found from the calibrations of Schus-ter&Nissen(1989)for stars bluer than(b?y)=0.550, and from the calibration for K2–M2dwarfs by Olsen (1984)for the redder stars.The calibrations by Schus-ter&Nissen are assumed to be valid for(b?y)<0.590. However,we decided to apply them for(b?y)<0.550 only,since beyond this value the calibrations yield spu-riosly high metallicites of0.45–0.75dex.On the other hand,the calibration by Olsen(1984)is valid for the range(b?y)>0.514,but it is rather uncertain for (b?y)>0.550,as it is based on a small number of stars with spectroscopic[Fe/H]determinations.Therefore,the accuracy of the metallicity determinations for the cooler stars is poorer than for the hotter objects.

Figure1shows the comparison between our derived photometric metallicities and spectroscopic metallicities taken from the literature(Cayrel de Strobel et al.1997, Favata et al.1997)for42dwarfs.It can be seen that the photometric and spectroscopic data are in good agreement with each other,especially when data by Favata et al. (1997)is used.

Characterization of the disk population has been made by applying the chemical criterion(see RPM for details), according to which stars with[Fe/H]

Table1.Metallicity distribution of218nearby K dwarfs ?1.150

?1.050

?0.950

?0.850

?0.753

?0.652

?0.555

?0.4511

?0.3518

?0.2539

?0.1539

?0.0536

0.0530

0.1528

0.256

0.351

H.J.Rocha-Pinto&W.J.Maciel:Consistent metallicity distributions amongst F,G and K dwarfs3

Particular care must be taken in the sense of avoiding any bias towards metal-poor stars in our sample.Some bias could be produced by intrinsic biases in the uvby databases we have used.From the218K dwarfs in our?-nal sample,138have photometric data from Olsen(1993), 40from Olsen(1994)and40from Hauck&Mermilliod (1998).It is di?cult to investigate the presence of any bias in the compilation by Hauck&Mermilliod,as it con-tains objects from several heterogeneous sources.On the other hand,the samples in Olsen’s papers are very well de-scribed and di?erent subsamples are easily identi?ed,par-ticularly in Olsen(1993).Three subsamples of this last catalogue are present in our sample:G5-type HD stars, calibration stars and high-velocity stars.Biases could be present in the calibration stars due to selection e?ects, and high-velocity stars which are likely to be old metal-poor stars.Of the138stars in our sample taken from Olsen(1993),38are G5-type HD stars,77are calibration stars and23are high-velocity stars.The average metallic-ity of G5-type stars is around?0.19dex,while the cali-bration and high-velocity stars have average metallicites of?0.10and?0.07dex,respectively.The average metal-licity of the stars coming from the catalogues of Olsen (1994)and Hauck&Mermilliod(1998)is around?0.15 dex.The standard deviation of the metallicity distribu-tions of all these subsamples is0.21–0.23dex.Therefore, no bias towards metal-poor objects is likely to be present in our sample.The di?erences in the metallicity distri-bution of the subsamples may suggest a small bias to-wards metal-rich objects.However,these di?erences may be caused by the fact that the subsamples have di?erent (b?y)ranges,some of which depend more strongly on the di?erent metallicity calibrations we used.

The resulting metallicity distribution is presented in Table1.It can be seen that no stars have[Fe/H]

https://www.wendangku.net/doc/3c17821732.html,parison of the metallicity distributions of

F,G,and K dwarfs

Figure2shows a comparison between our K dwarf metal-licity distribution and that of the G dwarfs(RPM).It can be seen that there is a very good agreement between these distributions,with only some small di?erences in the range?0.7<[Fe/H]

1.The metallicity distribution of the F dwarf sample

studied by Twarog(1980),comprising936stars,af-ter applying corrections due to stellar evolution and scale height,assuming the Salpeter initial mass func-tion(IMF).Twarog’s(1980)sample was built with the primary purpose of studying the age–metallicity rela-tion.It is composed exclusively by F dwarfs,selected by T e?range,and is expected to be representative of our vicinity.Metallicities are found from uvby pho-tometry,but using a very simple calibration in which [Fe/H]depends linearly onδm1.

2.The metallicity distribution of Wyse&Gilmore

(1995),with128F and G dwarfs.Wyse&Gilmore (1995)use the same photometric calibrations as RPM.

The major di?erence between these works is that Wyse &Gilmore(1995)have used photometric data by Olsen (1983),while RPM have used the more recent data from Olsen(1993).This last paper is speci?cally con-cerned with G stars,while Olsen(1983)gives more attention to stars ranging from A0to G0.There-fore,their metallicity distribution includes some late

F dwarfs,apart from the

G dwarfs.

3.The metallicity distribution of Flynn&Morell(1997),

comprising179G and K dwarfs,after applying the chemical criterion.They have built their sample from

G and K dwarfs,listed in CNS3,with(R?I)mea-

surements and Geneva photometric indices available in the literature.Their sample has179stars with [Fe/H]≥?1.2after applying the chemical criterion, from which97are G dwarfs and82are K dwarfs.In order to improve the statistics of their database,we have used the metallicity distribution for their com-bined sample of G and K dwarfs.

4.The metallicity distribution derived by Rocha-Pinto

&Maciel(1998),based on the chromospheric activity survey(Soderblom1985;Henry et al.1996),with730 dwarfs of types late F,G and early K.All stars in the chromospheric activity survey are expected to be located within50pc from the Sun,and are mostly

G dwarfs,with some late F and early K dwarfs.

Str¨o mgren photometric indices for these stars were taken from Olsen(1983,1993,1994)and used to?nd metallicities adopting the same calibrations used here.

All these distributions use metallicities estimated by photometric data.However,they di?er in the selection criteria and calibrations used.In spite of these di?erences, the agreement of the metallicity distributions(Figures2

4H.J.Rocha-Pinto &W.J.Maciel:Consistent metallicity distributions amongst F,G and K dwarfs

https://www.wendangku.net/doc/3c17821732.html,parison between the metallicity distributions

for K dwarfs (this work)and G dwarfs (RPM).

https://www.wendangku.net/doc/3c17821732.html,parison of the G dwarf metallicity distribution (RPM)and other distributions in the literature.Table 2.Fraction of dwarfs with [Fe/H]

and 3)is very good.The fraction of stars with

[Fe/H]

Note also that all distributions,except that by Flynn &Morell (1997),show a prominent single peak around ?0.20dex.As shown by Rocha-Pinto &Maciel (1997b),this fea-ture could be explained by an intense star formation era

from 5to 8Gyr ago.Therefore,the main conclusion that can be drawn from the comparisons above is that there is a remarkable consistency amongst the distributions of F,G and K dwarfs.This consistency could only be attained if the chemical enrichment and star formation history have been essentially the same for all late-type dwarfs .

4.Correction factors owing to chromospheric activity The raw data of the metallicity distributions are often sub-ject to a variety of corrections due to observational errors,cosmic scatter and scale height e?ects.When a sample has stars with lifetimes lower than the disk age,correc-tions due to stellar evolution must also be applied.Such corrections are needed to convert the observed metallicity distribution into the true distribution.

For a distribution based on spectroscopic [Fe/H],these corrections are generally su?cient.However,for pho-tometric distributions there is an additional correction which has been totally neglected in past studies.This cor-rection is needed in order to take into account the e?ects of the chromospheric activity on the photometric indices.

By studying the metallicity distribution in a sample of 730late-type dwarfs with varying levels of chromospheric activity,Rocha-Pinto &Maciel (1998)have shown that,for the active stars,the di?erence between the spectro-scopic and the photometric metallicity increases system-atically as a function of the stellar activity.This result is a consequence of the m 1de?ciency,which is more pro-nounced in active binaries (Gim′e nez et al 1991),but ac-tually seems also to be present in normal active stars (Gi-ampapa et al.1979;Basri et al.1989;Morale et al.1996).A metallicity distribution that does not take into account this e?ect will be biased towards metal-poor stars.The elimination of identi?ed active stars from the sample is not an ideal solution to this problem as,in single late-type dwarfs,the activity is linked to the stellar age (Soderblom et al.1991).Samples free of active stars will be also free of young stars,which will introduce another bias,in the sense of avoiding the expected metal-richer dwarfs.Even if there was no relation between age and activity,there would always remain some unidenti?ed active stars in the photometric surveys,as we do not know how to identify such stars from their indices.The only way to keep a minimum compromise between the achievement of a non-biased sample and an accurate metallicity distribution is to make use of approximate corrections for the e?ects of the chromospheric activity.

The corrections we are proposing assume that all active

stars,for which the chromospheric index log R ′

HK >?4.75(Soderblom et al.1991),have photometric metallicities lower than the spectroscopic values by a constant amount

?.In fact,?is likely to depend on log R ′

HK ,but for the

H.J.Rocha-Pinto&W.J.Maciel:Consistent metallicity distributions amongst F,G and K dwarfs5

Table3.Metallicity distribution for active stars and cor-rections

?1.150000

?1.050000

?0.950000

?0.850000

?0.750.00508?0.00009?0.01?0.01

?0.650.01015?0.00096?0.08?0.06

?0.550.01523?0.00685?0.58?0.44

?0.450.02030?0.03097?2.63?2.00

?0.350.09645?0.08674?7.37?5.60

?0.250.20305?0.14168?12.04?9.14

?0.150.26396?0.10795?9.17?6.97

?0.050.203050.02736 2.32 1.77

0.050.096450.1349511.468.71

0.150.071070.1270010.798.19

0.250.010150.06311 5.36 4.07

0.350.005080.01884 1.60 1.22

0.4500.003520.300.23

∞?4.75χ(log R′HK)d log R′HK,(1)

whereχ(log R′HK)is the distribution of stellar chromo-spheric activity,that can be found from the combined data of Soderblom(1985)and Henry et al.(1996),and?is es-timated by using Eq.(5)of Rocha-Pinto&Maciel(1998). Using Eq.(1),we haveˉ?=0.149dex.

The normalized photometric metallicity distribution of the active stars,D([Fe/H]),from Rocha-Pinto&Maciel (1998),is shown in Table3.Instead of identifying the active stars in the data sample,the approach we have taken here assumes that a fraction c of the total num-ber of stars in the sample(N tot)are active stars.There-fore,the number of active stars in each metallicity bin is cN tot D([Fe/H]),and to correct the metallicity distribu-tion,these active stars should be allocated to more metal-rich bins by an amount ofˉ?.

The fraction c is likely to depend on the spectral type considered,as the chromospheric activity is thought to be caused by the interaction between the stellar rotation and the convection in the stellar envelope.The decrease of the outer convective zone towards hotter stars indicates that young hotter stars do not show much activity(Elgar?y et al.1997).For a sample centered on G dwarfs,we can take c=0.296as a good value,according to Henry et al. (1996).

Table3also presents the normalized corrections r to the metallicity distribution.The numbers in the table were

found by the subtraction of D[Fe/H]from a gaussian curve ?tted to this distribution with a mean shifted byˉ?.These corrections are to be multiplied?rst by cN tot,before they can be added to the metallicity distribution,and before the application of any other corrections due to observational errors,cosmic scatter,stellar evolution or scale height.

The absolute corrections to the G dwarf metallicity dis-tribution of RPM and the K dwarf distribution derived in this work are shown in the last columns of Table3,where r K=rcN tot(K)and r G=rcN tot(G)with N tot(K)=218 and N tot(G)=287.Note that we have assumed the same values for c andˉ?for G and K dwarfs,as there is no information about their dependence on the stellar mass.

It should be stressed that these corrections are valid only for distributions binned by0.1dex,with each bin centered at the metallicities presented in the?rst column of Table3,and for[Fe/H]determined by Str¨o mgren pho-tometry.In order to apply them to a distribution binned in a di?erent way,we provide the equations below:

r X=0.296δz N tot(X) G([Fe/H]?ˉ?)?G([Fe/H]) ,(2) whereδz is the bin size in dex,assumed constant,and

G([Fe/H])=

1

2π

exp ?([Fe/H]?μ)2

6H.J.Rocha-Pinto&W.J.Maciel:Consistent metallicity distributions amongst F,G and K dwarfs Fig.4.δm1as a function of the chromospheric activity

for the active stars in the sample of Rocha-Pinto&Maciel

(1998).G dwarfs and K dwarfs are marked by solid and

open circles,respectively.

Table4.Activity indices for common stars in the Einstein

and chromospheric activity survey

HD105?4.36?3.58

HD166?4.33?3.43

HD25680?4.54?3.93

HD97334?4.40?4.06

H.J.Rocha-Pinto&W.J.Maciel:Consistent metallicity distributions amongst F,G and K dwarfs7

1.Low mass stars would preferably form in higher metal-

licity clouds,due to the e?cient cooling driven by the radiation of molecules containing metals.

2.The Catalogue of Nearby Stars could have a metallicity

bias,in the sense of favouring metal-rich stars amongst the cooler ones.

In what follows,we shall examine these hypotheses sep-arately.

5.1.Metal-enhanced star formation of K dwarfs

The?rst hypothesis resembles the metal-enhanced star formation model(MESF;Talbot&Arnett1973;Talbot 1974;see also Tinsley1975,1980).This model was pro-posed to explain the lack of metal-poor G dwarfs,when the G dwarf problem was identi?ed.The idea of Favata et al.(1997),although not explicitly stated in this way,is that stars of progressively lower masses are generally born with metallicities above than average,just like a mass-dependent metal-enhanced star formation.

There are problems with this hypothesis.If MESF could produce a lack of metal-poor K dwarfs compared to G dwarfs,then the same reasoning indicates that there would be a paucity of metal-poor G dwarfs compared to F dwarfs,and so on.It is not possible to test this hy-pothesis using stars earlier than F0,since the older earlier stars have already evolved away from the main sequence. However,the F dwarf metallicity distribution corrected by stellar evolution(Twarog1980)is not di?erent from the distribution of the G dwarfs in the metal-poor range (see Figure3).The F dwarf metallicity distribution could have another intrinsic bias towards metal-rich stars due to the accretion of Jupiter-mass planets(Laughlin&Adams 1997).However,the extent of these e?ects is not presently known.Moreover,as there is a metallicity gradient in the Galaxy(see for example Maciel and K¨o ppen1994),the fraction of cooler dwarfs related to the other stars should increase towards the Galactic center.Studies of the varia-tion of the IMF as a function of galactocentric radius show just the opposite(Scalo1986;Matteucci&Brocato1990).

Figure5compares the metallicity distributions found by Favata et al.(1997)with the G dwarf(RPM)and our present K dwarf metallicity distributions,after the appli-cation of the corrections due to chromospheric activity. These corrections were not applied to these distributions in the previous?gures,since we were comparing photo-metric distributions,which are expected to be a?ected in the same way by chromospheric activity.However,to com-pare a photometric distribution with a spectroscopic one, the corrections in Table3are needed.The G dwarf metal-licity distributions show a good agreement(upper panel of Figure5),except for[Fe/H]>+0.10,where the dis-tribution by Favata et al.(1997)shows a larger number of metal-rich stars.The same occurs in the K dwarf dis-tribution(lower panel of Figure5).Note also the lack of metal-poor K dwarfs in the sample by Favata et al.(1997) compared to ours.This di?erence is not likely to be caused

by errors in the photometric calibrations we have used, since Figure1demonstrates the good agreement with the spectroscopic metallicities,which is even closer for their

data.

The MESF model was not successful in giving a rea-sonable explanation to the G dwarf problem,as it requires both very large chemical inhomogeneities in the interstel-

lar medium and very ine?cient star formation in metal-poor regions(Tinsley1980).Our present knowledge of star formation and initial mass function corroborates this,as

we shall show below.

Padoan et al.(1997)have recently presented analytical expressions for the initial mass function(IMF)taking into account the dependence of the star formation on the physi-

cal parameters of the molecular clouds.Their model shows that cooler clouds form preferably lower mass stars.The

IMF has a single maximum and an exponential cuto?be-low it.For the idea of Favata et al.to be valid,regions with [Fe/H]

below1M⊙,and in more metal-rich clouds the IMF cut-o?should lie beyond0.6–0.7M⊙.Using the expressions given by Padoan et al.(1997),and taking average values

for cloud density and velocity dispersion,the temperature of the clouds for such cuto?s should be22K and19–17 K,respectively.This is hotter than the mean tempera-ture expected for typical dark clouds,8–15K(Goldsmith 1988).However,according to Lin(1997),at the present metallicity of the globular clusters([Fe/H]<～?1.0dex), the cold dense clouds could cool to around10K,putting the IMF cuto?at0.2M⊙,according to the formulae by Padoan et al.(1997).

Even if the IMF cuto?were around0.9–1M⊙in the hotter clouds,there would be no such a direct relation be-tween the metallicity and the cloud temperature.The tem-perature in a molecular cloud is not solely determinated by the cooling rate(which can depend on the metallicity), but it depends also on the cloud density and on the exis-tence of internal and external heating sources(Goldsmith 1988;Cernicharo1991).A di?erence of5K,as that re-quired for the IMF cuto?to be1M⊙or0.6M⊙,could exist even inside the same cloud,where the metallicity is likely to be the same everywhere,as shown by Young et al. (1982)and Cernicharo(1991).There is no strong evidence that the star formation mechanisms would be di?erent for G and K dwarfs.The bump at0.7M⊙in the present-day mass function,quoted by Favata et al.(1997)as an evi-dence favouring a bimodality in the star formation of low mass stars,was more easily explained by Kroupa et al. (1990)as a real feature in the mass–magnitude relation due to the e?ects of the increasing importance of H?as an opacity source.Given the considerations above,it is reasonable to conclude that MESF cannot account for the lack of metal-poor K dwarfs in the sample by Favata et al.(1997).

8H.J.Rocha-Pinto&W.J.Maciel:Consistent metallicity distributions amongst F,G and K dwarfs

Fig.6.Sources for the parallaxes in the Third Catalogue of Nearby Star(Gliese&Jahrei?1991).

Fig.7.The real inclusion limit of the CNS3as a function of[Fe/H]and(B?V)for UBVRI parallaxes.The curves correspond to(B?V)of0.5,0.6,0.7,0.8and0.9.The labels indicate the curves for the cooler and hotter stars.

5.2.A metallicity bias in the catalogue of nearby stars According to Favata et al.(1997),the use of photometric parallaxes could introduce a metallicity bias in the CNS2. Note,however,that our sample does not show this prob-lem,in analogy with the K dwarf metallicity distribution found by Flynn&Morell(1997).The samples by RPM and Flynn&Morell were also selected from the Catalogue of Nearby Stars,although both papers have considered a more recent version.

We decided to investigate the parallax sources in CNS3.This version of the catalogue was used instead of CNS2,as all recent work on the metallicity distributions is based on it.Moreover,any bias in the CNS2would also be present in the CNS3,since both catalogues were built in the same fashion.We begin by selecting all stars with(B?V)between0.5and1.4,as in Favata et al. (1996).The sample was further divided into‘G stars’and ‘K stars’at(B?V)=0.8.There are1421objects in this colour range,from which550are G stars and871 K stars.Figure6shows the number of stars included in the CNS3according to the parallax sources.These sources are:(i)trigonometrical parallaxes;(ii)spectroscopic par-allaxes and parallaxes determined from broad-band pho-tometric colours;(iii)photometric parallaxes determined from uvby colours;(iv)photometric parallaxes determined from other photometric systems;and(v)photometric par-allaxes for white dwarfs.As can be seen,the main sources for the CNS3are the trigonometrical parallaxes,and par-allaxes determined from spectral types or UBVRI colours (which we will call UBVRI parallaxes).The contribution by photometric parallaxes at this colour range is negli-gible.Both the spectroscopic and UBVRI parallaxes are determined from mean calibrations built using the stars for which accurate trigonometric parallaxes are available (Gliese&Jahrei?1989).As these calibrations include stars with varying chemical composition,this must refer to an average metallicity.At a given colour,metal-poor stars have higher absolute magnitudes than their richer coun-terparts,because their main sequences lay below that of the average-metallicity stars in the colour-magnitude dia-gram.Therefore,metal-poor stars would be estimated to be systematically farther away than they really are by the use of spectroscopic and UBVRI parallaxes,as Favata et al.(1997)suggested.Could this e?ect be large enough to introduce a metallicity bias in the CNS3?

In order to investigate this problem,we need to know how the‘25pc limit’for inclusion in the CNS3depends on the metallicity as well on the colour of the stars by using an average colour–magnitude relation.We have used the theoretical zero-age main sequences(ZAMS)calculated by VandenBerg(1985).His ZAMS for[Fe/H]=?0.23 was chosen as the mean ZAMS,since this metallicity cor-responds roughly to the average metallicity of the solar neighbourhood stars(cf.RPM).In Figure7,we show the real limit for inclusion in the CNS3,for(B?V)colours ranging from0.50to0.90.The?gure shows that metal-poor stars,with[Fe/H]

We have looked for such e?ects in the data by compar-ing the distances from the CNS3with the distances mea-sured by the HIPPARCOS satelite,both for stars with trigonometric and UBVRI parallaxes.The sample of G and K dwarfs,built according to the prescriptions above, was further divided into four samples:(i)G dwarfs in-cluded in the CNS3with trigonometric parallaxes(here-after tG);(ii)G dwarfs with spectroscopic and UBVRI parallaxes(ubvG);(iii)K dwarfs included with trigono-metric parallaxes(tK);and(iv)K dwarfs with spectro-scopic and UBVRI parallaxes(ubvK).The number of stars with distances in both the CNS3and in the HIPPAR-COS database is236(tG),204(ubvG),262(tK)and272 (ubvK).

H.J.Rocha-Pinto&W.J.Maciel:Consistent metallicity distributions amongst F,G and K dwarfs9 Fig.8.Stellar Distances from the CNS3and from the HIPPARCOS database,for di?erent stellar groups de?ned by their parallax sources.The dot-dashed lines at the bottom panels separate stars with good distance estimates in the CNS3from those assumed to be closer than they are.

Figure8shows a comparison of the CNS3and HIP-PARCOS distances of these four groups.A number of trends can be seen in these panels.Let us consider?rst the two groups included in the CNS3with trigonometric parallaxes,tG and tK.It is possible to see that the agree-ment between the CNS3and HIPPARCOS distances im-proves as we consider stars closer to the Sun,re?ecting the better accuracy of ground-based parallax measurements of nearby objects.A very small number of stars was also included in the catalogue in spite of having trigonomet-ric parallaxes smaller than0.039.There are nearly10% of the stars in each group tG and tK that are located much farther away than25pc.This is due to errors in the parallax measurements,so that we do not expect any chemical composition di?erences between those stars and the stars with accurate distances.The situation is di?er-ent for the groups ubvG and ubvK,whose distances are shown in the bottom panels of Fig.8.For these groups,the scatter around the line of same distance does not depend on the actual stellar distance.Such scatter is very likely to be produced by the varying chemical composition of these stars.There is a group of stars with underestimated distances in CNS3,both amongst the G and K dwarfs.We separate these stars by a dot-dashed line.The possibility that the inclusion of metal-rich stars in CNS3with UB-VRI parallaxes has an important e?ect can be checked by comparing the metallicity of the stars at both sides of the dot-dashed lines in the bottom of Fig.8.

To estimate the metallicities we used the same proce-dures described in Section2.The number of stars with metallicities in each subgroup is:185(tG),176(ubvG), 111(tK)and121(ubvK).The number of stars deviating from the line of same distance is21G dwarfs and20K dwarfs.

In Figure9,we show the metallicity distributions of the groups tG,ubvG,tK and ubvK.There is no indica-tion that the metallicity distribution of G stars is di?er-ent at the extreme metallicities,regardless of the parallax source.However,the metallicity distribution of the group ubvG has a remarkable single peak at[Fe/H]～?0.20dex, which is not present in group tG.This peak is also appar-ent in the metallicity distributions discussed in Section2, but it is not clear whether it is caused by something re-lated to the colour–magnitude calibration,since it is also present in Twarog’s(1980)distribution which uses very di?erent selection criteria.On the other hand,the metal-licity distributions of K dwarfs seem to depend strongly on the parallax sources of the CNS3.A Kolmogorov-Smirnov test indicates that both distributions are di?erent at a signi?cance level of99.99%.However,the di?erence oc-curs in the opposite sense of what we were expecting as group tK shows much more metal-rich objects than the group ubvK.Also there seems to be more metal-poor stars

10H.J.Rocha-Pinto&W.J.Maciel:Consistent metallicity distributions amongst F,G and K dwarfs

https://www.wendangku.net/doc/3c17821732.html,parison of the metallicity distributions of the stellar groups included in the CNS3with di?erent parallax sources:a)groups tG e ubvG;b)groups tK and ubvK. amongst the ubvK dwarfs.Therefore,these groups do not show any bias derived from UBVRI parallaxes,although some excess of metal-rich stars is apparent in the group of K dwarfs with trigonometric parallaxes.

However,this result is not conclusive,since the metal-licity distribution of group tK is more strongly dependent on the calibration by Olsen(1984)than group ubvK(the fraction of stars in these groups that have(b?y)>0.550 is0.55and0.37,respectively).It is worth to note that the metallicity distribution of group ubvK agrees better with the groups of G dwarfs.The hypothesis that the metal-licity distribution of group ubvK is the same as those of groups ubvG and tG can only be rejected at a signi?cance level of0.2246and0.2339,respectively.

It is then particularly important to see whether there are di?erences amongst the groups of deviating stars,that is,those objects to the right of the dot-dashed lines in Fig.8,and the remaining groups.The metallicites of the deviating G stars range from?0.5to+0.1dex,with an average around?0.10dex.There is no indication that this group has more metal-rich stars compared to the others. The absence of stars with metallicites lower than?0.5 dex can well be ascribed to the size of the sample.As an illustration,the KS test gives signi?cance levels of0.517 and0.314for this distribution not to be taken from the same population of groups ubvG and tG,respectively.The situation is di?erent for K dwarfs.The group of deviating K dwarfs has metallicities ranging from?1.6to?0.05dex,with an average around?0.65dex.This result is very peculiar since it suggests that the stars which have systematically underestimated distances in the CNS3are metal-poor,while we would expect that metal-poor stars would have overestimated distances according to Figure 7.However,this question cannot be properly answered because the metallicity of the group of deviating K dwarfs also strongly depends on the metallicity calibration for stars cooler than(b?y)=0.550.

In spite of that,if such bias is likely to be present in the catalogue,it should occur for both G and K dwarfs,being in fact stronger for the hotter stars.The non-existence of such bias amongst the G dwarfs,which have even more accurate photometric metallicites,indicates that it does not a?ect the content of the CNS3.This can happen be-cause the limit for inclusion of objects in the CNS3due to spectroscopic and UBVRI parallaxes is more?exible than the limit for trigonometric parallaxes.This is evident from Figure8.In this plot we see that there are many stars in the CNS3whose distances in this catalogue are greater than25pc,amongst those included with UBVRI paral-laxes.Thus,in the CNS3there is not a?xed limit at25 pc for the inclusion of stars with UBVRI parallaxes,and there seems to be no corresponding metallicity-bias.

The simplest hypothesis to account for the results found by Favata et al.(1997)is that their sample is not representative of the galactic population of K dwarfs,due to its small size.The original sample randomly selected from the CNS2,and consisting of around100G and100 K dwarfs(Favata et al.1996),can be expected to be rep-resentative.However,the number of stars that were e?ec-tively observed is63G dwarfs and26K dwarfs.As Favata et al.(1997)themselves state,relatively fewer cooler stars were observed due to their faint magnitudes.This observa-tional selection is not likely to remove the representative-ness of a large data sample.However,small samples are much easily a?ected by statistical?uctuations due to the elimination of some stars.This can explain why the dis-tributions by Favata et al.(1997)show large?uctuations and not a single prominent peak as the other metallicity distributions in the literature.

Acknowledgements.HJR-P thanks Mar′?lia Sartori for some helpful discussions.We are indebted to Dr.E.H.Olsen for some important remarks on an earlier version of this paper. We have made use of the SIMBAD database,operated at CDS, Strasbourg,France.This work has been partially supported by F APESP and CNPq.

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-2.0-1.5-1.0-0.50.00.5

-2.0

-1.5

-1.0

-0.5

0.0

0.5

Favata et al. (1997)

Cayrel de Strobel et al. (1997)

p h o t o m e t r i c [F e /H ]

spectroscopic [Fe/H]

-1.2

-1.0

-0.8

-0.6

-0.4

-0.2

0.0

0.2

0.4

0.6

-0.02

0.000.020.040.060.080.100.120.14

0.160.180.20 This work (K dwarfs) RPM (G dwarfs)

R e l a t i v e n u m b e r

[Fe/H]

-1.2

-1.0

-0.8

-0.6

-0.4

-0.2

0.0

0.2

0.4

0.00

0.05

0.10

0.15

0.20

0.25

0.30

RPM

Twarog (1980)

Wyse & Gilmore (1995)

Rocha-Pinto & Maciel (1998) Flynn & Morell (1997)

R e l a t i v e n u m b e r

[Fe/H]

-4.8

-4.6

-4.4

-4.2

-4.0

-3.8

-0.10

-0.05

0.00

0.05

0.10

0.15

0.20

K dwarfs G dwarfs

δm 1

log R'HK

Trig. Parallaxes

Spect. Types & Broad Phot.Phot. Parallaxes (uvby)Phot. Parallaxes (other)

White Dwarfs

G stars

K stars

501001502002503003504004500

50100150200250300350400450

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0.25

K dwarfs

This work

Favata et al. (1997)

R e l a t i v e n u m b e r

[Fe/H]

-1.2-1.0-0.8-0.6-0.4-0.20.00.20.40.6

0.00

0.05

0.10

0.15

0.20

G dwarfs

RPM after correction Favata et al. (1997)

R e l a t i v e n u m b e r

[Fe/H]

-1.0

-0.8

-0.6

-0.4

-0.2

0.0

15.0

17.5

20.022.525.027.530.0

0.5

0.5

0.9

i n c l u s i o n l i m i t i n C N S 3 (p c )

[Fe/H]

25

50

75

100

125

0510152025303540

455055G dwarfs included with UBVRI parallaxes (ubvG)

C N S 3

D i s t a n c e s (p c )

Hipparcos Distances (pc)

25

50

75

100

125

0510152025303540

455055G dwarfs included with trigonometric parallaxes (tG)

C N S 3

D i s t a n c e s (p c )

Hipparcos Distances (pc)

50

100

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0510152025303540

455055(740 pc)

K dwarfs included with UBVRI parallaxes (ubvK)

C N S 3

D i s t a n c e s (p c )

Hipparcos Distances (pc)

50

100

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0510152025

303540

455055(699 pc)

K dwarfs included with trigonometric parallaxes (tK)

C N S 3

D i s t a n c e s (p c )

Hipparcos Distances (pc)

青年教师基本功大赛演讲稿

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聚合诸侯捍卫中原，匡正天下功业千秋。号令诸侯以匡周室，主要靠的不是 武力。 行为磊落不欺诈，美德流传于身后。孔子赞美齐桓公，也称赞管仲。 百姓深受恩惠，天子赐肉与桓公，命其无拜来接受。桓公称小白不敢，天子 威严就在咫尺前。 晋文公继承来称霸，亲身尊奉周天王。周天子赏赐丰厚，仪式隆重。 接受玉器和美酒，弓矢武士三百名。晋文公声望镇诸侯，从其风者受尊重。 威名八方全传遍，名声仅次于齐桓公。佯称周王巡狩，招其天子到河阳，因 此大众议论纷纷。 赏析 《短歌行》 (“周西伯昌”)主要是曹操向内外臣僚及天下表明心 迹，当他翦灭群凶之际，功高震主之时，正所谓“君子终日乾乾，夕惕若 厉”者，但东吴孙权却瞅准时机竟上表大说天命而称臣，意在促曹操代汉 而使其失去“挟天子以令诸侯”之号召， 故曹操机敏地认识到“ 是儿欲据吾著炉上郁!”故曹操运筹谋略而赋此《短歌行 ·周西伯 昌》。 西伯姬昌在纣朝三分天下有其二的大好形势下， 犹能奉事殷纣， 故孔子盛称 “周之德， 其可谓至德也已矣。 ”但纣王亲信崇侯虎仍不免在纣王前 还要谗毁文王，并拘系于羑里。曹操举此史实，意在表明自己正在克心效法先圣 西伯姬昌，并肯定他的所作所为，谨慎惕惧，向来无愧于献帝之所赏。 并大谈西伯姬昌、齐桓公、晋文公皆曾受命“专使征伐”。而当 今天下时势与当年的西伯、齐桓、晋文之际颇相类似，天子如命他“专使 征伐”以讨不臣，乃英明之举。但他亦效西伯之德，重齐桓之功，戒晋文 之诈。然故作谦恭之辞耳，又谁知岂无更讨封赏之意乎 ?不然建安十八年(公元 213 年)五月献帝下诏曰《册魏公九锡文》，其文曰“朕闻先王并建明德， 胙之以土，分之以民，崇其宠章，备其礼物，所以藩卫王室、左右厥世也。其在 周成，管、蔡不静，惩难念功，乃使邵康公赐齐太公履，东至于海，西至于河， 南至于穆陵，北至于无棣，五侯九伯，实得征之。 世祚太师，以表东海。爰及襄王，亦有楚人不供王职，又命晋文登为侯伯， 锡以二辂、虎贲、斧钺、禾巨 鬯、弓矢，大启南阳，世作盟主。故周室之不坏， 系二国是赖。”又“今以冀州之河东、河内、魏郡、赵国、中山、常 山，巨鹿、安平、甘陵、平原凡十郡，封君为魏公。锡君玄土，苴以白茅，爰契 尔龟。”又“加君九锡，其敬听朕命。” 观汉献帝下诏《册魏公九锡文》全篇，尽叙其功，以为其功高于伊、周，而 其奖却低于齐、晋，故赐爵赐土，又加九锡，奖励空前。但曹操被奖愈高，心内 愈忧。故曹操在曾早在五十六岁写的《让县自明本志令》中谓“或者人见 孤强盛， 又性不信天命之事， 恐私心相评， 言有不逊之志， 妄相忖度， 每用耿耿。

2008年浙师大《外国文学名著鉴赏》期末考试答案

（一）文学常识 一、古希腊罗马 1．（1）宙斯(罗马神话称为朱庇特)，希腊神话中最高的天神，掌管雷电云雨，是人和神的主宰。 （2）阿波罗，希腊神话中宙斯的儿子，主管光明、青春、音乐、诗歌等，常以手持弓箭的少年形象出现。 （3）雅典那，希腊神话中的智慧女神，雅典城邦的保护神。 （4）潘多拉，希腊神话中的第一个女人，貌美性诈。私自打开了宙斯送她的一只盒子，里面装的疾病、疯狂、罪恶、嫉妒等祸患，一齐飞出，只有希望留在盒底，人间因此充满灾难。“潘多拉的盒子”成为“祸灾的来源”的同义语。 （5）普罗米修斯，希腊神话中造福人间的神。盗取天火带到人间，并传授给人类多种手艺，触怒宙斯，被锁在高加索山崖，受神鹰啄食，是一个反抗强暴、不惜为人类牺牲一切的英雄。 （6）斯芬克司，希腊神话中的狮身女怪。常叫过路行人猜谜，猜不出即将行人杀害；后因谜底被俄底浦斯道破，即自杀。后常喻“谜”一样的人物。与埃及狮身人面像同名。 2．荷马，古希腊盲诗人。主要作品有《伊利亚特》和《奥德赛》，被称为荷马史诗。《伊利亚特》叙述十年特洛伊战争。《奥德赛》写特洛伊战争结束后，希腊英雄奥德赛历险回乡的故事。马克思称赞它“显示出永久的魅力”。 3．埃斯库罗斯，古希腊悲剧之父，代表作《被缚的普罗米修斯》。6．阿里斯托芬，古希腊“喜剧之父”代表作《阿卡奈人》。 4．索福克勒斯，古希腊重要悲剧作家，代表作《俄狄浦斯王》。5．欧里庇得斯，古希腊重要悲剧作家，代表作《美狄亚》。 二、中世纪文学 但丁，意大利人，伟大诗人，文艺复兴的先驱。恩格斯称他是“中世纪的最后一位诗人，同时又是新时代的最初一位诗人”。主要作品有叙事长诗《神曲》，由地狱、炼狱、天堂三部分组成。《神曲》以幻想形式，写但丁迷路，被人导引神游三界。在地狱中见到贪官污吏等受着惩罚，在净界中见到贪色贪财等较轻罪人，在天堂里见到殉道者等高贵的灵魂。 三、文艺复兴时期 1．薄迦丘意大利人短篇小说家，著有《十日谈》拉伯雷，法国人，著《巨人传》塞万提斯，西班牙人,著《堂?吉诃德》。 2．莎士比亚，16-17世纪文艺复兴时期英国伟大的剧作家和诗人，主要作品有四大悲剧——《哈姆雷特》、《奥赛罗》《麦克白》、《李尔王》，另有悲剧《罗密欧与朱丽叶》等，喜剧有《威尼斯商人》《第十二夜》《皆大欢喜》等，历史剧有《理查二世》、《亨利四世》等。马克思称之为“人类最伟大的戏剧天才”。 四、17世纪古典主义 9．笛福，17-18世纪英国著名小说家，被誉为“英国和欧洲小说之父”，主要作品《鲁滨逊漂流记》，是英国第一部现实主义长篇小说。10．弥尔顿，17世纪英国诗人，代表作：长诗《失乐园》，《失乐园》，表现了资产阶级清教徒的革命理想和英雄气概。 25．拉伯雷，16世纪法国作家，代表作：长篇小说《巨人传》。 26．莫里哀，法国17世纪古典主义文学最重要的作家，法国古典主义喜剧的创建者，主要作品为《伪君子》《悭吝人》（主人公叫阿巴公）等喜剧。 五、18世纪启蒙运动 1）歌德，德国文学最高成就的代表者。主要作品有书信体小说《少年维特之烦恼》，诗剧《浮士德》。 11．斯威夫特，18世纪英国作家，代表作：《格列佛游记》，以荒诞的情节讽刺了英国现实。 12．亨利·菲尔丁，18世纪英国作家，代表作：《汤姆·琼斯》。 六、19世纪浪漫主义 （1拜伦， 19世纪初期英国伟大的浪漫主义诗人，代表作为诗体小说《唐璜》通过青年贵族唐璜的种种经历，抨击欧洲反动的封建势力。《恰尔德。哈洛尔游记》 （2雨果，伟大作家，欧洲19世纪浪漫主义文学最卓越的代表。主要作品有长篇小说《巴黎圣母院》、《悲惨世界》、《笑面人》、《九三年》等。《悲惨世界》写的是失业短工冉阿让因偷吃一片面包被抓进监狱，后改名换姓，当上企业主和市长，但终不能摆脱迫害的故事。《巴黎圣母院》 弃儿伽西莫多，在一个偶然的场合被副主教克洛德.孚罗洛收养为义子，长大后有让他当上了巴黎圣母院的敲钟人。他虽然十分丑陋而且有多种残疾，心灵却异常高尚纯洁。 长年流浪街头的波希米亚姑娘拉.爱斯梅拉达，能歌善舞，天真貌美而心地淳厚。青年贫诗人尔比埃尔.甘果瓦偶然同她相遇，并在一个更偶然的场合成了她名义上的丈夫。很有名望的副教主本来一向专心于"圣职"，忽然有一天欣赏到波希米亚姑娘的歌舞，忧千方百计要把她据为己有，对她进行了种种威胁甚至陷害，同时还为此不惜玩弄卑鄙手段，去欺骗利用他的义子伽西莫多和学生甘果瓦。眼看无论如何也实现不了占有爱斯梅拉达的罪恶企图，最后竟亲手把那可爱的少女送上了绞刑架。 另一方面，伽西莫多私下也爱慕着波希米亚姑娘。她遭到陷害，被伽西莫多巧计救出，在圣母院一间密室里避难，敲钟人用十分纯朴和真诚的感情去安慰她，保护她。当她再次处于危急中时，敲钟人为了援助她，表现出非凡的英勇和机智。而当他无意中发现自己的"义父"和"恩人"远望着高挂在绞刑架上的波希米亚姑娘而发出恶魔般的狞笑时，伽西莫多立即对那个伪善者下了最后的判决，亲手把克洛德.孚罗洛从高耸入云的钟塔上推下，使他摔的粉身碎骨。 （3司汤达，批判现实主义作家。代表作《红与黑》，写的是不满封建制度的平民青年于连，千方百计向上爬，最终被送上断头台的故事。“红”是将军服色，指“入军界”的道路；“黑”是主教服色，指当神父、主教的道路。 14．雪莱，19世纪积极浪漫主义诗人，欧洲文学史上最早歌颂空想社会主义的诗人之一，主要作品为诗剧《解放了的普罗米修斯》，抒情诗《西风颂》等。 15．托马斯·哈代，19世纪英国作家，代表作：长篇小说《德伯家的苔丝》。 16．萨克雷，19世纪英国作家，代表作：《名利场》 17．盖斯凯尔夫人，19世纪英国作家，代表作：《玛丽·巴顿》。 18．夏洛蒂?勃朗特，19世纪英国女作家，代表作：长篇小说《简?爱》19艾米丽?勃朗特，19世纪英国女作家，夏洛蒂?勃朗特之妹，代表作：长篇小说《呼啸山庄》。 20．狄更斯，19世纪英国批判现实主义文学的重要代表，主要作品为长篇小说《大卫?科波菲尔》、《艰难时世》《双城记》《雾都孤儿》。21．柯南道尔，19世纪英国著名侦探小说家，代表作品侦探小说集《福尔摩斯探案》是世界上最著名的侦探小说。 七、19世纪现实主义 1、巴尔扎克，19世纪上半叶法国和欧洲批判现实主义文学的杰出代表。主要作品有《人间喜剧》，包括《高老头》、《欧也妮·葛朗台》、《贝姨》、《邦斯舅舅》等。《人间喜剧》是世界文学中规模最宏伟的创作之一，也是人类思维劳动最辉煌的成果之一。马克思称其“提供了一部法国社会特别是巴黎上流社会的卓越的现实主义历史”。

外国名著赏析论文

题目：浅析从简爱到女性的尊严和爱 学院工商学院 专业新闻学3 学号 姓名闫万里 学科外国文学名着赏析 [摘要] 十九世纪中期，英国伟大的女性存在主义先驱，着名作家夏洛蒂勃朗特创作出了她的代表作--《简爱》，当时轰动了整个文坛,它是一部具有浓厚浪漫主义色彩的现实主义小说，被认为是作者"诗意的生平"的写照。它在问世后的一百多年里，它始终保持着历史不败的艺术感染力。直到现在它的影响还继续存在。在作品的序幕、发展、高潮和结尾中，女主人公的叛逆、自由、平等、自尊、纯洁的个性都是各个重点章节的主旨，而这些主旨则在女主人公的爱情观中被展露的淋漓尽致，它们如同乌云上方的星汉，灼灼闪耀着光芒，照亮着后来的女性者们追求爱情的道路。? [关键词] 自尊个性独特新女性主义自由独立平等 《简爱》是一部带有自转色彩的长篇小说，它阐释了这样一个主题：人的价值=尊严+爱。从小就成长在一个充满暴力的环境中的简爱，经历了同龄人没有的遭遇。她要面对的是舅妈的毫无人性的虐待，表兄的凶暴专横和表姐的傲慢冷漠，尽管她尽力想“竭力赢得别人的好感”，但是事实告诉她这都是白费力气的，因此她发出了“不公平啊！--不公平！”的近乎绝望的呼喊。不公平的生长环境，使得简爱从小就向往平等、自由和爱，这些愿望在她后来的成长过程中表现无疑，

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青年教师基本功大赛即兴演讲题目【题目1】我的兴趣爱好【题目2】谈谈内心和谐【题目3】人最难超越的高度就是自己【题目4】我的价值观【题目5】谈谈与人相处【题目6】坚守心灵的一方沃土【题目7】给快乐找个理由【题目8】年轻 没有什么不可以【题目9】心底无私天地宽【题目10】人是需要一点精神的【题目11】我们与时代同行【题目12】生活从“心”开始【题目13】让更多的人快乐 【题目14】面对繁杂的教学工作 你如何调整心态 【题目15】和谐、健康、快乐【题目16】我喜爱的书刊【题目17】你如何发展自己的专业弱点【题目18】善待自己 呵护希望【题目18】.上公开课对一个教师的成长的作用【题目19】培养积极心态 感悟责任人生【题目24】永不言弃 我心永恒 准备时间 3分钟 【题目25】.你怎样做个身心健康的老师【题目26】你如何看待家长满意工程 【题目27】新课程执行过程中 你碰到最棘手的问题是什么【题目28】课堂教学中 你最关注的是什么【题目29】你希望学校领导关心青年教师哪些方面【题目30】谈谈自己的业余生活【题目31】简评最近的工作情况。【题目32】怎样才能提高教师的凝聚力。【题目33】.谈谈做班主任的心得【题目34】.你怎样定义教师【题目35】简介杨森中学【题目36】.点评一位我校的优秀教师【题目37】.如何看待家长的不理解【题目38】.谈谈卫生与健康【题目39】谈谈我校的环境. 【题目40】谈谈如何管理学生【题目41】谈谈你对职业道德的认识【题目42】我参加校本研修之感想。【题目43】“依法治教 注重服务 着力塑造行业形象” 请你谈谈你的设想【题目44】.如何发挥你校师生之特长 【题目45】.怎样调动老师的工作积极性 【题目46】.谈谈你对校本教研的看法。【题目47】.我是怎样备课的。【题目48】.维持校门口的秩序 我的一点想法。【题目49】如何丰富教师的业余生活 缓解教师的心理压力 【题目50】谈谈你对节日文化的认识【题目51】学校活动很多的情况下 你如何调节自己的心态 【题目52】德育倡导“全面德育 全员德育” 请你谈谈自己的理解。【题目53】如何让家长尊重教师 【题目54】你认为提高教育质量应从哪里抓起【题目55】从哪些方面帮助班主任管理学生篇二：教师即兴演讲题目之63个话题 教师即兴演讲题目之63个话题 来源：思雨教育资源网|教学资源|课件论文|作文作者：无边思雨发表日期：2009-5-30 13:16:19 阅读次数： 910 查看权限：普通文章 1、如何维护班集体荣誉？ 2、如何看待学生时代早恋问题？ 3、成人与成才二者是怎样的关系？结合实例说明自己的观点。 4、不同地域、不同背景、不同习惯的同学之间该如何相处？ 5、怎样面对学习、生活中遇到的挫折？ 6、你最崇拜的人是谁？“名人”还是自己？ 7、你认为我们是否应有感恩之心？感恩于谁？ 8、你希望自己会是怎样一位老师？你会如何教育自己的学生？ 9、“言行、仪表”与个人的发展。 10、如今继续提倡“勤俭、节约”作风是否已过时？ 11、在各种资料、媒体中常讲张扬个性，你认为我们该张扬什么样的个性？ 12、三轮车工人方尚礼自己生活的如乞丐，却将自己蹬车收入的35万多元用来资助失学儿童，当病重时，社会捐助给他治病的钱，也被他捐给了希望工程。你对方尚礼的这种行为有何评述？ 13、电视广告不宜过多 14、保护环境是每个人的责任