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Comparative study of the two large flares from SGR1900+14 with the BeppoSAX Gamma-Ray Burst

a r X i v :a s t r o -p h /0312062v 1 2 D e c 2003

Astronomy &Astrophysics manuscript no.0511February 2,2008

(DOI:will be inserted by hand later)

Comparative study of the two large ?ares from SGR1900+14

with the BeppoSAX Gamma-Ray Burst Monitor

C.Guidorzi 1,F.Frontera 1,2,E.Montanari 1,3,M.Feroci 4,L.Amati 2,E.Costa 4,and M.Orlandini 2

Dipartimento di Fisica,Universit`a di Ferrara,via Paradiso 12,I-44100Ferrara,Italy

2Istituto di Astro?sica Spaziale e Fisica Cosmica,CNR,Sezione di Bologna,via Gobetti 101,I-40129Bologna,Italy 3ISA “A.Venturi”,Modena,Italy

Istituto di Astro?sica Spaziale e Fisica Cosmica,CNR,Sezione di Roma,via Fosso del Cavaliere,I-00133Roma,Italy

Received Accepted ...

Abstract.We report on spectral and temporal results of the 40–700keV observations,obtained with the Gamma-Ray Burst Monitor (GRBM)on board BeppoSAX ,of the two large ?ares from the Soft Gamma-ray Repeater SGR 1900+14occurred on August 27,1998and April 18,2001.From their intensity,?uence and duration,the ?rst one was classi?ed as “giant”and the second as “intermediate”.The spectral results have been obtained with an improved response function of the GRBM.We ?nd that the two events have similar spectral properties,but different temporal properties.The major difference concerns the time pro?les of the light curves,whereas the lack of evidence in the 2001?are for the erratic time variability found at high frequencies (10–1000Hz)in the 1998?are could be ascribed to lower counting statistics.We discuss these results in the light of the magnetar model proposed for SGR sources.

Key words.pulsars:individual (SGR1900+14)–X–rays:?ares –stars:magnetic ?elds

1.Introduction

Soft-Gamma Repeaters (SGRs,see Hurley 2000and Woods 2003for reviews)are X–/gamma–ray transient sources that unpredictably undergo periods of bursting activity,separated by sometimes long intervals (from years to decades)of quies-cence.

To date,the SGR class includes four sources (SGR0525?66,SGR1627?41,SGR1806?20and SGR1900+14)plus two candidates,SGR1801?23(only two bursts detected;Cline et al.2000)and SGR1808?20(one SGR-like burst observed;Lamb et al.2003).All con?rmed SGRs,on the basis of their early determined positions,appeared to be associated with young supernova remnants (SNRs)of ages ≤104yr.However,basing on more precise locations,in most cases this association has been questioned (Lorimer &Xilouris 2000;Hurley et al.1999a;Kaplan et al.2002a)and in some cases attributed to random chance (Gaensler et al.2001).All SGRs appear to be in our galaxy,except for SGR0525-66which is in the Large Magellanic Cloud.

Typically,bursts from SGRs have short durations(～0.1s),recurrence times of seconds to years,energies of ～1041D 210ergs (D =10D 10kpc).Their hard X–ray spectra (>25keV)are analytically consistent with an Optically Thin Thermal Bremsstrahlung (OTTB )with temperatures of 20–40keV .During quiescence,persistent X-ray emission (<10keV)has been observed from all of them with luminosities of ～

1035–1036D 210erg s

and power-law spectral shapes.In the case of SGR1900+14,an additional blackbody (BB )component (kT bb ～0.5keV)is requested (Woods 2003).SGR1806?20and SGR1900+14,during quiescence,show X-ray pulsations with periods in the range from 5to 8s and spin-down rates of ～10?11?10?10s/s (see,e.g.,Hurley et al.1999b,Kouveliotou et al.1999).From these sources,also evidence of X–ray lines has been reported during bursts:an emission line at ～6.4keV from the former source (Strohmayer &Ibrahim 2000)and an absorption–like feature at ～5keV from the latter (Ibrahim et al.2002).

Rarely,“giant”?ares of hard X–/γ–rays have been observed from SGR0525-66(Mazets et al.1979)and SGR1900+14(Cline et al.1998;Feroci et al.1999;Hurley et al.1999a;Mazets et al.1999b).They show du-rations of hundreds of seconds,pulsations during most part of the event,and peak luminosities in excess of 1044D 210erg/s.

After large bursts fading afterglow emission has been ob-served.A fading X–ray afterglow,visible for several days,has been discovered after the large ?ares from SGR1900+14(i.e.,the giant ?are of August 1998and the intermediate ?are of April 2001,see below).The X–ray afterglow decays as a power-law (F (t )∝t ?α)with temporal index α～0.7after the August 1998event (Woods et al.2001)and α～0.9after the April 2001event (Feroci et al.2003).The X-ray afterglow spectrum is the combination of a power-law (PL )and a BB ,with

2Guidorzi et al.:Large?ares from SGR1900+14with BeppoSAX

the BB not visible at early times when the PL component is predominant,but emerging at later times,when the PL compo-nent becomes weaker(Woods et al.1999a;Feroci et al.2003), suggesting that the non-thermal component fades more rapidly than the thermal one(see also Lenters et al.2003,for the X-ray tail that followed the short burst occurred on April28,2001). The presence of X–ray afterglow emission from the other SGR sources is still an open question.Radio afterglow has also been observed from SGR1900+14after the August1998event by Frail et al.(1999),who detected a transient radio source with the Very Large Array telescope at the source position following the giant?are.This is the only point-like radio source associ-ated to an SGR to date.

On the basis of their locations and temporal properties and the absence of companion stars,SGRs have been proposed to be young(<104yrs)isolated neutron stars(NS)with ultra-strong magnetic?elds(B dipole>1014gauss),a.k.a.“mag-netars”.The magnetar model(Duncan&Thompson1992; Thompson&Duncan1993;Thompson&Duncan1995)con-siders a young neutron star with a very strong magnetic?eld (～1014?1015G),whose decay powers the quiescent X-ray emission through heating of stellar crust,while the low-level seismic activity and the persistent magnetospheric currents (Thompson et al.2002)occasionally cause big crustquakes which trigger short bursts and large?ares.In the magnetar sce-nario,the absorption feature from SGR1806-20can be inter-preted as ion-cyclotron resonance in the huge magnetic?eld of the NS(Ibrahim et al.2002).

SGRs share some properties(pulse period distribution, spin-down rate,lack of a companion star,quiescent X-ray lu-minosity)with a peculiar class of neutron stars,the so–called anomalous X-ray pulsars(AXPs,see,e.g.,Mereghetti1999 for a review).Additional evidence for a link between the two classes has been provided by the detection of SGR-like bursting activity also from the AXPs1E2259+586(Kaspi et al.2002, 2003)and1E1048.1-5937(Gavriil et al.2002),and from the recent discovery of an absorption–like feature at～8.1keV from the AXP1RXS J170849?400910(Rea et al.2003).

1.1.SGR1900+14

SGR1900+14was discovered in1979following three bursts in two days(Mazets et al.1979).After its discovery,the source was found bursting again in1992(Kouveliotou et al.1993) and,after?ve years of quiescence,in May1998,when it entered an extremely active bursting period,that reached its maximum with the above mentioned giant?are of August 27,1998.A precise localization of the source with IPN (Hurley et al.1999c)showed that SGR1900+14lays just out-side a Galactic SNR,G042.8+00.6and could be asso-ciated with it.However,recently Kaplan et al.(2002b) found three new candidate SNRs(G043.5+00.6,G042.0-00.1 and G041.5+00.4),that could be related to SGR1900+14 as well.Observations of the quiescent soft X–ray coun-terpart(Vasisht et al.1994)have shown a 5.16-s periodic-ity with a spin-down rate of10?10s/s(Hurley et al.1999b; Kouveliotou et al.1999).

Several measurements of the quiescent spectrum have

been performed(e.g.,Hurley et al.1999b,Kouveliotou et al.1999).An X–ray observation with the BeppoSAX satellite

(Woods et al.1999a)shows that the0.1-10keV quiescent spec-

trum can be described by a photoelectrically absorbed(N H～1.8×1022cm?2)BB(kT bb～0.5keV)plus a PL with a photon

indexΓ=1.1±0.2.

The source spectrum during the standard bursting activity has been mainly observed in the hard(>20keV)X–/gamma–

ray band.Results reported by Mazets et al.(1999a)from Konus–Wind observations show that the burst photon spec-

tra can be analytically described by an OTTB model(I(E)∝

E?1exp(?E/kT))with kT～20?30keV with no signif-icant spectral evolution within a single event or from event

to event.Only in the case of a few bursts,discussed by

Woods et al.(1999b),the spectrum is better described by the smoothly broken power-law,widely used to describe GRB

spectra(Band et al.1993).In these cases also a soft-to-hard spectral evolution has been observed,with hardness/intensity

anticorrelation.

The giant?are occurred on1998August27(here af-ter GF98)was observed with the Konus–Wind spectrome-

ter(Cline et al.1998;Mazets et al.1999b),the Ulysses burst

monitor(Hurley et al.1999a)and the BeppoSAX GRBM (Feroci et al.1999).The5.16-s periodicity,along with its har-

monics(e.g.,Feroci et al.1999and2001,hereafter F99 and F01,respectively),was clearly detected during the?are.

Mazets et al.(1999b)?nd the spectrum well described with an OTTB model with temperature kT evolving rapidly(in about1 s and in a non-monotonic way)from>300keV to～20keV.

Feroci et al.(1999)?nd a more complex40–700keV spec-

trum(OTTB,with kT～31keV,plus PL with photon index Γ～1.5)in the early part(?rst68s)of the event which evolves to an OTTB-like shape(kT～29keV)at late times(last128 s).At that time,as pointed out by F99,the response function of the BeppoSAX GRBM was not well known at large instru-mental off–axis angles,in the direction of which the source was observed,and thus a systematic error of10%was tenta-tively added to the statistical uncertainties.By joining together the BeppoSAX GRBM spectra with the20–150keV Ulysses data(F01),also affected by similar systematics,the?rst128-s spectrum after the68s from the?are onset was?t by two BB, with kT bb1～9keV and kT bb2～20keV,plus a PL model with photon indexΓ～2.8,while the later128-s spectrum was bet-ter described by an OTTB model with kT～29keV,consistent with the F99results.

After the giant?are of1998August27and the recurrent

bursting activity prolonged until1999(Mazets et al.1999a), the source entered a period of quiescence for more than two years,which ended on2001April18,when another large?are (hereafter IF01)with a shorter duration and intermediate inten-sity occurred.Due to a simultaneous proton solar burst,both the Ulysses burst monitor and the Konus–Wind spectrometer were overwhelmed by a high count rate.The only instrument which provided high-time resolution data of the event was the BeppoSAX GRBM(Guidorzi et al.2001a;2001b).

An improved response function of the BeppoSAX GRBM

is now available(see below)for all off–axis angles.In this pa-

Guidorzi et al.:Large ?ares from SGR1900+14with BeppoSAX 3

per we present the results of the spectral analysis of the 2001?are,the reanalysis of the spectral data of the 1998giant ?are with the new GRBM response function,and the results of the Power Spectral Density (PSD)estimate of the high-frequency (up to 1kHz)?ux variations of the source during the two ?ares.

Preliminary results of this analysis were reported elsewhere (Guidorzi et al.2003a).

2.The BeppoSAX GRBM

The Gamma-Ray Burst Monitor (GRBM;Frontera et al.1997;Feroci et al.1997)is one of the instruments on board the BeppoSAX satellite (Boella et al.1997)operative through June 1996and April 30,2002.The GRBM consisted of four op-tically independent CsI(Na)units forming a square box:each unit had a geometric area of ～1136cm 2.GRBM units No.1and 3were co-aligned with the Wide Field Cameras (WFC’s;Jager et al.1997).The data continuously available from the GRBM included 1-s ratemeters in the 40–700keV and >100keV energy channels,225–channel spectra in the 40–700keV band integrated over 128s and,in the case of burst trigger,7.8125-ms ratemeters for 96s and,for 10s after the trigger,～0.5-ms count rates,both in the 40–700keV band.From the 1-s ratemeters,it is possible to extract the source 40–100keV and 100–700keV count rates under the assumption that the source ?ux above 700keV is negligible (see Amati et al.1999).The detection units,except for the units 1and 3within small off–axis directions (Amati et al.1999),were surrounded,in a complex way,by materials of the BeppoSAX payload.In order to exploit the capabilities of the GRBM units 2and 4and those of units 1and 3at large off–axis angles,the com-plete GRBM response function was derived with Monte Carlo methods (Rapisarda et al.1997,Calura et al.2000).Recently the complete response has been tested with the Crab Nebula and with several GRBs which were observed,at different in-strument off–axis angles,with both the GRBM and the BATSE experiment (e.g.,Guidorzi 2002,Guidorzi et al.2003b,Costa &Frontera 2003),with the limitation of a generally smaller sta-tistical accuracy of the GRBM data,with respect to the BATSE data.The deconvolution results of the GRBs,in terms of de-rived GRB direction and photon spectrum,are in excellent agreement with those obtained with BATSE.Thus we expect that systematic errors,also for possible terrestrial albedo ef-fects,are similar to those which affect the deconvolution of the BATSE data (e.g.,Paciesas et al.1999).Actually,we must point out that the total counts measured for the brightest GRBs detected with both GRBM and BATSE and used to test the GRBM response function,amount to a few 105cts in the most illuminated GRBM unit (e.g.,～250,000for GRB990123,～140,000for GRB991216,～130,000for GRB971110),while about 8×105cts were collected in the GRBM unit 1due to GF98.Due to the smallest statistical uncertainties in the latter case,the systematics could have a major in?uence on de-convolution results.

Fig.1.1-s background subtracted light curves of the two ?ares in the 40–700keV energy band.Top :2001April 18event;bot-tom :1998August 27event.The 5.2-s modulation is apparent in both cases.Vertical dotted lines mark the 128-s intervals during which 225-channel spectra were accumulated on board.

3.Observations and data analysis

GF98triggered the GRBM on August 27,1998at 10:22:15.7UT,while IF01triggered the GRBM on April 18,2001at 07:55:11.5UT.IF01occurred when the SGR1900+14line of sight was only ～11?off–axis from the detection unit No.1(indeed the ?are was initially observed also with the WFC No.1;Guidorzi et al.2001a,2001b,Feroci et al.2003).GF98oc-curred when the line of sight to the source was at high off–axis angles:an elevation angle of 48?with respect to the GRBM equatorial plane,an azimuthal angle of 29?with respect to the GRBM unit 1axis,and 61?with respect to unit 4axis.All GRBM units detected the event,with the best signal given by unit 1.Our results,except when expressly stated,will be based on the data obtained from this unit.

The background subtracted light curves of both ?ares are shown in Fig.1,where the onset time is used as zero time.Details of the observation of the GF98event can be found in the paper by F01.The time duration of IF01was 40s,whereas

4Guidorzi et al.:Large ?ares from SGR1900+14with BeppoSAX

GF98lasted about 300s.The 7.8125-ms ratemeters cover the entire IF01.The 0.5-ms ratemeters are available for the interval 0.69–10.69s from the ?are onset.During IF01,the background level was fairly stable and was evaluated by linear interpola-tion of the background levels in time intervals [-50,-10]s and [+50,+150]s,before and after the ?are,respectively.

For the spectral analysis of IF01,the available data are two 225–channel 128-s contiguous

spectra.The start and end times of these spectra are reported in Table 1.The interval A covers ～97%of the ?are ?uence;the interval B includes little more than the isolated pulse at t ～40s from the ?are onset (see Fig.1).

The available data for the spectral analysis of GF98are three spectra in three contiguous 128-s intervals (A,B,C)de-scribed in Table 1.The A spectrum includes both the initial hard spike and the intermediate smooth decay,whereas the B and C spectra include the 5.16-s pulsation modulated decay (see Fig.1).

To get the source spectra,we subtracted from the above data a background spectrum of the same duration (128s)inter-polated between those measured before and after the ?are.The spectra were analyzed with the XSPEC software pack-age (Arnaud 1996).The quoted errors are given at 90%con?-dence level (CL)for one parameter (?χ2=2.7),except when otherwise speci?ed.

4.Results 4.1.Light curves

The light curves of both ?ares are complex and different from each other.As it can be seen from Fig.1,unlike GF98,IF01does not shows any initial spike;the time duration of IF01is much shorter than GF98,ending after about 40s when a four-peaked repetitive pattern sets up in GF98(F01).The light curves show measured counts,that do not account for the dif-ferent effective areas of the two ?ares:actually,the effective area corresponding to the direction of GF98was about 1/3that of IF01.

In order to better compare the time behaviour of IF01with that of GF98during the early phase,in Fig.2we show the light curves of both events in the ?rst 40s.Even if some similari-ties between the two light curves could be found,in the ?rst 8seconds they are markedly different.Apart from the GF98ini-tial spike,which is not observed in IF01,in the ?rst 3seconds,IF01shows a ?rst weak peak,which does not have a corre-spondence with any peak of the GF98light curve.From the two light curves it is also unclear to which phase of the IF01light curve the GF98initial spike corresponds.We have con-sidered two possible correspondence cases:i)the GF98ini-tial spike time corresponds to the fast rise of the IF01light curve (duration ?t rise =0.25±0.05s)at 3s from the ?are onset (Fig.3),ii)the dips corresponding to the interpulses in both light curves are aligned (see Fig.4).In the ?rst case (see Fig.3),we ?nd that all IF01dips soon after each peak are separated from the assumed main rise at multiple distances of ～https://www.wendangku.net/doc/932327681.html,ing Fourier techniques,after detrending the data stretch by ?tting with a trapped-?reball model (see Fig.19),

Fig.2.Background subtracted light curve of IF01compared with the corresponding ?rst 40s of GF98in the 40–700keV energy band.Top:IF01;bottom :GF98.Vertical dotted lines mark the 5.2-s intervals and are synchronized with the IF01pulsations.

the best estimate of this periodicity in the time intervals from 2to 7,is P 01=5.21±0.05s (negligible barycenter correc-tion),a value which is consistent with that measured from the observation of the X-ray quiescent source soon after the event (P quiesc =5.17284268s)(Woods et al.2003).In GF98the dips have period P 98circa 5.16s (F99),but they are out of phase with respect to the initial spike.

In the second case (see Fig.4),the result is that the GF98initial spike corresponds to the peak of the weak pulse preced-ing the ?rst dip (and the main rise)of the IF01light curve.

In both cases,it is possible to see that,when the pulse peak fades away (slice 7of Fig.3or 4),the corresponding dip is no more visible.The pattern completely changes soon before IF01ends (slice 8):while the continuum level seems to fade under the GRBM sensitivity,a pulse rises up to a peak count rate of about 160counts in 31.25ms,the same level as the early pulse.The pulse does not seem to have properties similar to the preceding regular pulses:it neither occurs in phase with them nor exhibits a similar structure.

The complexity of the GF98and IF01light curves and their mutual differences are better apparent in Fig.6,which,for cor-respondence case ii),shows them split into 9panels,each dis-playing a single pulsation cycle,with 125ms time resolution.The pulse shape of the IF01pulsation and its evolution are ap-parent in the panels from 2to 7.Two pulses and two dips nearly equally spaced are visible in the pulse shape,with the second pulse stronger and fading later and almost suddenly in panel 7.

Guidorzi et al.:Large?ares from SGR1900+14with BeppoSAX5 Table1.Time intervals of the available128-s count spectra.

2001April18(IF01)A?94.67+33.33

B+33.33+161.33

1998August27(GF98)A?59.6+68.4

B+68.4+196.4

C+196.4+324.4

6Guidorzi et al.:Large ?ares from SGR1900+14with

BeppoSAX

Fig.6.Pulse shape evolution of both ?ares (IF01:black ,GF98:red )during the ?rst nine slices.The time offset between the two events was chosen in order to align the ?rst interpulses (see also Fig.4).Horizontal scale :phase of rotation cycle;vertical scale :counts per 125ms.

-200

0 200 400 600 800 1000

1200 1400 1600 1800-10

C t s / s

Time (s)

IF01 (>100 keV)

Fig.7.IF01light curve in the >100keV energy band.The fact that the pulse preceding the main rise is also apparent in this band,seems to suggest that it is unlikely to be a precursor.

tected by Konus (Mazets et al.1999b)in the energy channels above 50keV ,while the IF01pulse is detected by the GRBM even above 100keV (see Fig.7).

4.3.Erratic time variability

A temporal analysis of the 40–700keV data with Fourier tech-niques was performed for each of the two ?ares.In the case of the 1998?are,we limited the analysis to the ?rst 38s when the 5.2-s periodicity was not well set up yet.We exploited both available time binnings of 7.8125ms and,for the ?rst 10s,～0.5ms.

Using the longer time binning,for IF01we estimated the PSD function of the entire light curve in the 0.031–64Hz fre-quency range.The resulting PSD,inclusive of the Poissonian variance,is shown in Fig.8.We adopted the Leahy et al.(1983)normalization,such that the Poissonian noise level has a PSD value of 2.As can be seen from this ?gure,apart from two ap-parent peaks at 0.2and 0.4Hz due to the ～5.2-s periodicity,the main PSD feature is its strong decrease with frequency.It mainly depends on the fact that the light curve we are analyzing is a non-stationary process.

Indeed,in the null hypothesis that the light curve is a non-stationary Poisson process x (t )of duration T and mean value given by the deterministic function λ(t ),the mean PSD of the process at frequency f ,S x (f )=S λ(f )+2

(1)

where S λ(f )is the power spectrum of λ(t )(Leahy et al.1983normalization adopted).Actually,the PSD of a non-stationary

Guidorzi et al.:Large ?ares from SGR1900+14with BeppoSAX

Fig.8.Measured PSD of IF01using as time binning 7.8125ms.Solid line :PSD of the best-?t exponential function used to de-scribe the mean light curve of IF01,excluding the precursor (see text).Dashed line :Poissonian level corrected for the dead time.

process can also be in?uenced by other effects,like the detec-tor dead time (τ=4μs in our case),and the binning time (co-incident with the sampling time).For low frequencies (f ?f τwhere f τ=1/(2πτ)),as in our case (Nyquist frequency f N =64Hz),the dead time changes the PSD level by a factor (1?μτ)2,where μis the average measured count rate (Frontera &Fuligni 1978;see also van der Klis 1989).The dead time ef-fect,consistently with an expected correcting factor of 0.949(from the mean count rate μ

=6412cts/s)is visible in the Poissonian level shown in Fig.8.

Following the working scheme adopted by Frontera &Fuligni (1979),we have tested the null hypothesis that the measured PSD can be entirely explained in terms of a non-stationary process.Assuming that the average behaviour of the IF01light curve can be described by an exponential λ(t )=AU (t )e ?kt ,where U (t )is the step function (time origin at the main rise of the ?are,see discussion above),and A and k are free parameters,the expected PSD is S λ(f )=2A 2/[μT (k 2+(2πf )2)].From the ?t to the light curve,we derived the best-?t parameters of the exponential and thus the PSD of the function S λ(f ).After the addition of the Poissonian statistics corrected for the dead time,the expected PSD is shown in Fig.8as con-tinuous line.As can be seen from this ?gure,S λ(f )dominates the PSD up to ～10Hz where it achieves the Poissonian level.We have found that the power in excess of S λ(f )is negligible even above 10Hz,with no evidence of a non-Poissonian noise up to 64Hz.A similar analysis,performed in the ?rst 10s after the trigger using the high-time resolution binning of ～0.5ms,has also given a negative result up to 1kHz (see Fig.9),with the conclusion that up to a frequency of 1kHz no signi?cant non-Poissonian noise is present in the time variability of IF01.Following the same guidelines adopted above for IF01,we performed the PSD estimate of the ?rst 38s of GF98after the initial spike.The resulting PSD is shown in Fig.10along with the S λ(f )(continuous line),obtained from the best-?t of the exponential function λ(t )to the data,plus the Poissonian level corrected for the dead time.As it can be seen,also in this case S λ(f )dominates the measured power spectrum up to ～10Hz,

Fig.9.20Hz–1kHz PSD of IF01measured in the time in-terval [+0.7,+10.7]s after subtraction of the non-stationary Poissonian noise dead-time corrected.

Fig.10.PSD of the ?rst 38s of GF98with time origin 1s af-ter the onset,in order to exclude the spike.The time binning used is 7.8125ms.Solid line :PSD of the best-?t exponential function used to describe the mean light curve.Dashed line :Poissonian level corrected for the dead time.

even if some evidence of an excess power over the non station-ary Poissonian noise is visible.

To avoid a contamination of the PSD from the non-stationary component,we focused on the high-frequency do-main deriving the PSD of the ?rst 8s after the spike,with high-time resolution binning (～0.5ms).The resulting PSD is shown in Fig.11,where it can be seen that,above 20Hz,S λ(f )gives a small contribution to the total power and,above 100Hz,does not contribute at all (see also the inset in Fig.11).

The excess power with respect to the non-stationary Poisson model in the 6–1000Hz for the GRBM unit 1is shown in Fig.12.As can be seen,this time a relevant resid-ual power is apparent up to 1kHz.The non–Poissonian spec-trum S np (f )in the range 10-1000Hz is well ?t with a power law (S np (f )∝f ?α)with α=0.74±0.18.An excess power has also been found in the PSD of the other GRBM units (2,3,and 4).The cumulative result is shown in Fig.13.A power-law still gives the best description of the non–Poissonian spectrum with a best-?t power-law index of 0.75±0.15,even though also a ?icker noise (S np ∝1/f )gives an acceptable ?t (χ2/dof =10.6/9).Using the power-law best-?t values,the total fractional variation (in RMS units)in the range 10–1000Hz comes out to be around 1%.Concerning IF01,as far

8Guidorzi et al.:Large ?ares from SGR1900+14with

BeppoSAX

Fig.11.PSD of GF98in the time interval [+1,+9]s.Continuum line :PSD of the best-?t exponential function used to describe the ?rst 10s of the mean light curve.Dashed line :Poissonian level corrected for dead time.Inset :zoomed high-frequency

PSD.

Fig.12.PSD of the residual noise of GF98in the time interval [1,9]s.Solid line :best-?t power-law (see text).

as we assume similar fractional variability,we could not detect it because of the worse statistics;therefore,we cannot rule out the presence of similar non–Poissonian noise with comparable power for IF01.

4.4.Spectral properties

The two available source count rate spectra (A and B)of IF01and

the three (A,B,and C)source spectra of GF98are shown in Fig.14and Fig.15,respectively.For GF98,the A spectrum (inclusive of the initial spike)is well determined up to 700keV ,the B spectrum up to ～500keV and the C spectrum up to 200keV .As far as IF01is concerned,the spectrum A is well determined up to 700keV ,while the B spectrum can only be estimated up to 100keV .In the following,we limited our anal-ysis to the energy bands where signi?cant source counts were detected.

Several single,two–component and three–component mod-els were tested to ?t these spectra.In the case of the A spectrum of IF01,models like a power-law PL ,a cutoff power law (CUT -OFFPL ),a single BB ,an OTTB with or without a power-law PL ,are unsatisfactory,even in the 40–300keV energy band.Up to 300keV ,a BKNPL plus either a BB or an OTTB give

Fig.13.PSD of GF98for the interval [+1,+9]s averaged over the four GRBM units.Solid line :best-?t power law (see text).

Fig.14.Count rate spectra of IF01and their ?t with a BB +BKNPL during the interval A,and with a BB model during the interval B.The residuals to the models are shown as well.

a good ?t (χ2/dof =56/65with BB and χ2/dof =61/65with OTTB ).Also the sum of two BB cannot be ruled out (χ2/dof =72.6/66).In the top panel of Fig.14we show the ?t of the A spectrum with the BB plus BKNPL model.Clearly,an excess to the model is apparent in the 300–700keV band.The best ?t of the entire spectrum is obtained when a PL is added to either a BB +BKNPL model or an OTTB +BKNPL model.The best-?t parameters along with the χ2values are re-ported in Table 2,while in Fig.16(top)the EF (E )spectrum along with one of the best models (BB +BKNPL +PL )and the residuals to the model are shown.By adding a PL to the dou-ble BB ,the ?t goodness (χ2/dof =83/74)is also acceptable,

Guidorzi et al.:Large?ares from SGR1900+14with BeppoSAX

Fig.15.Count rate spectra of GF98and their?t with a BB+

BKNPL during the interval A and B,and with a BB model during

the interval C.The residuals to the model are shown as well.

even though worse than the?t with the two previous models,

with the following best-?t parameters:kT bb1=13.5+0.2

?0.2keV,

kT bb2=33+2?3keV,andΓ=?1.06+0.64

?0.03

The B spectrum(derived up to only100keV)can be?t with either a BB or an OTTB(χ2/dof=17.6/14andχ2/dof= 16.7/

14,respectively).The best-?t parameters are also reported in Table2,while the EF(E)spectrum and its best-?t model are shown in Fig.16(bottom panel).The multi-component models adopted for the A spectrum also yield acceptable?ts of this spectrum.

As far as the GF98spectra are concerned,?rst of all we caution that the results of the?ts of the A spectrum can be can be in?uenced by the dramatic dead-time and pile-up effects due to the hard initial spike contribution,the hardness of which Fig.16.EF(E)spectra of IF01.Top panel:A spectrum along

with the best?t with a BB+BKNPL+PL model.Bottom panel:

B spectrum along with the?t with a BB.Also the single model components and the residuals(in units ofσ)to the best-?t mod-

els are shown.

rapidly changes with time(see Mazets et al.1999b and also

F99).

In spite of that,the best?t of the A spectrum is obtained

using as input the three–component models which best?t the A spectrum of IF01:either a BB plus BKNPL plus PL or an OTTB plus BKNPL plus PL.The best-?t parameters along with theχ2values are also reported in Table2,while in Fig.17(top)

the EF(E)spectrum along with one of the best models(BB+ BKNPL+PL)and the residuals to the model are shown.The simple BB+PL or the OTTB+PL models,which were found to provide a good?t of the same spectrum with the prelimi-nary GRBM response function and the10%systematic error adopted by F99,with the improved response function provide unsatisfactory?ts(χ2/dof>2with dof=189).

The?t of the B spectrum was limited to the40–500keV energy band.The best-?t model is obtained with either a BB+BKNPL(χ2/dof=50.3/69)or an OTTB+BKNPL(χ2/dof= 50.7/69).However,in the latter case,the lower limit to the pho-ton indexΓ1cannot be constrained(see Table2).In agreement with the results by F01,we?nd that the OTTB+PL model,the BB+PL and the Band model(Band et al.1993)are de?nitely unacceptable(e.g.,χ2/dof=860/70for the former model). However,we?nd that also the double BB plus PL model,which was found by F01to provide the best?t to the GRBM plus Ulysses spectral data,does not provide a good?t to the40–

10Guidorzi et al.:Large?ares from SGR1900+14with BeppoSAX Table2.Best-?t parameters of the IF01and GF98photon spectra.

IF01A40–700BB+BKNPL+PL14.4+1.2

?0.82.1+0.1

?0.1

4.8+0.2

?0.2

73+2

OTTB+BKNPL+PL31.7+2.3

?2.10.6+0.2

?0.1

5.0+0.3

?0.2

73+1

?0.6+1.5

?0.6

64/72 1.2

B40–100BB12.7+1.6

?1.4

––––17.6/140.03

OTTB36+12

––––16.7/140.03

GF98A40–700BB+BKNPL+PL19+4

?31.0+0.2

?0.3

3.7+0.1

?0.1

75+1

6.4

OTTB+BKNPL+PL40+3?3?1.8+0.2

?0.63.48+0.02

?0.02

71+2

?2.1+1.1

?0.4

191/187>6.4

B40–500BB+BKNPL20.5+1.8

?1.81.3+0.2

?0.3

4.9+0.2

?0.1

75+2

–50.3/69 3.1

OTTB+BKNPL44+3?2

?0.372+1

–50.7/69 3.1

C40–200BB+PL16.0+0.4

?0.4

–––<2.641.3/360.49

Guidorzi et al.:Large ?ares from SGR1900+14with BeppoSAX

Fig.17.EF (E )average spectra of GF98.Top panel :A spec-trum with superposed the best-?t model BB +BKNPL +PL .Middle panel:B spectrum with superposed the best-?t model BB +BKNPL .Bottom panel :C spectrum with superposed the best-?t model BB +PL .Also the model components and the residuals to the best-?t models are shown.

～0.2Hz pulsation,with complex and variable shape of the pe-riodic pulses.The pulse shapes are different in the two cases.Only dips between pulses appear the common feature of both light curves.The most distinguishing feature of the GF98light curve is the presence of an initial spike,which is not observed in the case of IF01.In fact,given the dif?culty of justifying the

?rst weak pulse in the IF01light curve as a precursor (see Section 4.2),it appears that the initial GF98spike corresponds to this pulse (if the two events are assumed to be “phased”by their dips).This is one of the most important results of our com-parative analysis.

Fig.18.Time behaviour of the equivalent kT of an OTTB model for the entire duration of IF01and for the early part of GF98.Error bars are 90%CL.Top panel :GF98;bottom panel :IF01.

The periodicity found in the IF01light curve (P 01=5.21±0.05s)is consistent with that measured during the source quies-cence before and soon after the event (P quiesc =5.17284268s)(Woods et al.2003).

Within the magnetar model scenario (see F01,Thompson &Duncan 2001),the 1998giant ?are is triggered by a dis-tortion of the internal magnetic ?eld in the neutron star core,that induces large-scale fractures in the crust and strong mag-netic shears in the magnetosphere,that drive reconnection and conversion to Alf′v en waves.According to this view,the initial spike is the signature of a relativistic out?ow with a very low baryon load,as also suggested by the radio transient observed by Frail et al.(1999)and corroborated by the highly structured temporal pro?le of the spike,with peaks as narrow as ～10?2s (Mazets et al.1999b),whereas the pulsating tail would be due to the fraction (about 50%)of energy trapped in the magne-tosphere in the form of a photon-pair plasma.A similar sce-nario for the IF01time pro?le is clearly problematic:we do not see the spike.The spike absence could be explained in several ways.We focus on three possibilities:?rst,no huge energy re-lease comparable to that of GF98occurred;second,the spiking event occurred,but the beamed out?ow was not directed toward our line of sight;third,a comparable or slightly less energetic release really occurred,but the permanent changes undergone by the magnetosphere after the global recon?guration further to GF98(Woods et al.2001)are responsible for the unusual time pro?le of IF01.The ?rst explanation seems the most natural,

12Guidorzi et al.:Large?ares from SGR1900+14with BeppoSAX

since it easily accounts for the lower X–andγ-ray?uence of IF01and seems to agree with the minor changes observed in the trend of the

pulsation pro?le after the?are against what occurred after GF98(G¨o?g¨u s?et al.2002;Woods et al.2003). However the light curve of IF01shows some similarities(e.g., dips at the same phase in the correspondence case of Fig.4) to the initial stage of GF98.Furthermore,the pulse pro?le dur-ing IF01appears far more complex than it appeared at the later stages of GF98(Mazets et al.1999b)and than that of the quies-cent pulsar after1998(G¨o?g¨u s?et al.2002;Woods et al.2003). This suggests that a transient recon?guration of the magnetic ?eld took place related to this event,that caused the complex pulse pro?le evolution during the burst.In addition,the detec-

tion of a non-thermal X-ray afterglow after this event raises

the issue of a possible GRB-like mechanism for explaining this

emission(Feroci et al.2003;Ioka2001),that in turn would im-ply an out?ow of relativistic particles(whose signature is miss-

ing in IF01,however).

In the context of the magnetar model,F01pointed out that

the envelope of the light curve can give an important clue about the radiation emission mechanisms and/or the geometry during

the?ares.Thompson and Duncan(2001),assuming that the

emitted luminosity is the result of a cooling?reball trapped on the closed magnetic?eld lines of a neutron star,expect that

it varies as a power of the remaining?reball energy E a.As

a consequence the fading law of the radiation is expected to vary as L(t)=L(0)(1?t/t evap)a/(1?a),where t evap is the time

at which the?reball evaporates and its radius shrinks to zero, while a depends on the trapped?reball geometry and temper-

ature distribution(a=2/3or a=1/2in the case of spherical

or cylindrical geometry,respectively).F01found,for GF98, t evap=(501±13)s and a=0.828±0.005in the40–100 keV range,and t evap=(545±62)s and a=0.85±0.01in the100–700keV band.We?nd for the40–700keV the re-sult shown in Fig.19with the following best?t parameters:

t evap=(35.25±0.11)s,a=0.413±0.004.This result shows that,in contrast to the spherical-like geometry of GF98,the trapped?reball responsible for the pulsating tail of IF01had probably a cylinder-like geometry(a～1/2),with a non uni-form temperature distribution(that has the effect of decreasing the value of the?reball index a).

5.2.Erratic time variability

From the PSD estimates,it clearly emerges that GF98has time properties which are not observed in the case of IF01.A sig-ni?cant power above the Poissonian level is apparent up to 1kHz in the PSD of GF98,with a power-law shape(index α=0.75±0.15)with frequency.Even if the10–1000Hz frac-tional variation(in RMS units)is only1%,the PSD shows the clear presence of a?icker–like noise,similar to that observed in many accreting compact X–ray sources.

Barat et al.(1983)found evidence of timing noise in the X-ray decay of the March5burst from SGR0526-66,although in that case it was identi?ed as due to～23ms quasi-periodic os-cillations.An interpretation of the?icker–like noise in the light of the magnetar model is needed,although it could be possi-Fig.19.Light curve of IF01;the dashed line is the best?t with a ?reball model obtained for the time interval[7.46875,38.5]s, rebinned at5.171875s;the solid line shows the best?t ap-plied to the interval[3,38]s,whose parameters have been con-strained to vary within1σaround the best?t of the tail.

bly explained invoking the mechanisms described by Duncan (1998)and by Ioka(2001):they account for the ms quasi-periodicity as due to the excitation of global seismic oscilla-tions of the crust coupling strongly to Alf′v en modes in the lower magnetosphere.

A possible phenomenological interpretation of the detected noise is in terms of clustering of elementary pulses.In this case the noise dependence on frequency is determined by the distri-bution of waiting times between subsequent pulses and,possi-bly,by the distribution of the pulse intensity.There is a big va-riety of mechanisms that,in principle,may generate power-law noise withα≈1:see,e.g.,Kaulakys&Me?s kauskas(1998)and references therein.Davidsen&Schuster(2002)propose a sim-ple mechanism for generating pulse sequences with S(f)∝f?αin systems whose dynamics is driven by a variable threshold, like for earthquakes.This kind of mechanism is also known as an integrate-and-?re(IAF)model.It requires a threshold C(t) evolving with time according to a Brownian motion with dif-fusion constant D within a de?ned interval C l

In the light of the magnetar model,the observed noise could be the consequence of the dramatic energy release during the initial spike.Likely,the engine which powered the spike is far from equilibrium and the magnetic?eld lines probably undergo rapid and complex variations.If a threshold-controlled mech-anism,like that above described,is at work,unstable?reballs

Guidorzi et al.:Large?ares from SGR1900+14with BeppoSAX13 could be created,that burst whenever a particular threshold is

exceeded,that might depend on quantities like energy density,

magnetic?eld and its twist.In this scenario,the observed high-

frequency noise might be suggestive of how fractures in the

crust propagate with time.

5.3.Energy spectra

At?rst glance,we notice that the GF98spectrum of the?rst

40s is signi?cantly harder than that of IF01,as shown by the

comparison of the equivalent temperatures of an OTTB model.

However,unlike the discussed differences between the two

events,the spectral properties of GF98and IF01show strik-

ing similarities.In the time interval A,which covers most of

the IF01light curve and during the?rst68s of the GF98light

curve,both40–700keV spectra are best?t with the same three-

component models(BB+BKNPL+PL or OTTB+BKNPL+PL;

see Table2).Assuming the former of these models,both the BB

temperatures and break energies of the BKNPL model are sim-

ilar:kT98

bb =19+4?3keV and E98break=75+1?2keV,kT01bb=14.4+1.2

?0.8

keV and E01

break =73+2?2keV,respectively.However the cen-

troids of the BKNPL indices are only marginally consistent at 90%CL,and we remind that the A spectrum of GF98is likely distorted by dramatic dead-time and pile-up effects suffered during the initial spike.

The BB+BKNPL(+PL)model better agrees with the trapped?reball+corona scenario(Thompson&Duncan2001), at least in the case of GF98:the BB?ux remains almost con-stant throughout the?are,whereas the BKNPL and PL fade ex-hibiting a small spectral evolution.This is con?rmed also by the temporal evolution of the equivalent kT:while GF98ex-hibits a slow decrease during the?rst40s,after which it soft-ens even more slowly,IF01shows a mild increase followed at the end by a small drop,with no strong spectral evolution.In this scenario,the BB component is due to the outer layer of a trapped?reball,while the BKNPL can partially come from the surrounding corona,and,probably,from the reprocessing of the radiation coming from the inner?reball.Indeed such component,although it decreases,does not disappear in the time interval B of GF98,where the corona should already have evaporated.The BB temperature value in both GF98and IF01 are above the minimum photospheric temperature of a trapped ?reball expected in B>B QED magnetic?elds(eq.133from Thompson&Duncan1995).

While a possible interpretation can be given for the BKNPL, the origin of the high-energy(>300keV)power-law com-ponent,with positive index at least for the A spectra of both events,is more mysterious.

5.4.The last isolated pulse of IF01

The1.5-s long isolated pulse of IF01has a shape apparently different from that of the previous pulses.It is narrower and is not in phase with the previous ones.Thus,we are led to think about a different origin for it.A possibility is that,unlike the periodic light curve before it,whose likely origin is in the outer layer of the transient corona,the last pulse could originate in

100

150

200

250

-2-1 0 1 2 3 4 5 6 C

Time (s)

IF01 last pulse

Aug 29 1998

Fig.20.40–700keV time pro?les of the last isolated pulse of IF01(blue)and of the August29,1998burst(red).

the nearby of the neutron star surface and/or with the same mechanism of typical short bursts.We note that,the occurrence of short bursts during the tail of bright bursts was noted also in the tail of the August29event(Palmer2002).Actually,its average energy spectrum does not appear signi?cantly different from the A spectrum,and Fig.18shows that its kT is consistent with general behaviour at previous times.Thus,the last pulse mainly differs from the?rst part of the?are for its temporal properties rather than for its energy spectrum.

Actually,if we compare this pulse with the peculiar burst of August29,1998(Ibrahim et al.2001),also detected with the GRBM(see Fig.20),we?nd a similar light curve,even if the?uence of the IF01last pulse(～5×10?6erg cm?2)is about twice as high as that of the August29burst?uence in the 40–700keV band.Curiously,the duration of the subpulse of the August29burst is similar to that of the last pulse of IF01. This similarity could suggest a common origin of the last pulse of IF01with some of the brightest short bursts recorded from SGR1900+14.

6.Conclusions

The BeppoSAX GRBM was the only instrument that in the same40–700keV energy band allowed a detailed study of the two large X–/gamma–ray?ares from SGR1900+14occurred on1998August27and2001April18.In this paper we have compared the spectral and temporal properties of both?ares to study their similarities and distinctive features.Apart from the different time durations of the two?ares(～40s for IF01and ～300s for GF98)and a higher(>10)40–700keV?uence of GF98,other distinctive features have also been derived from our analysis.The light curve of IF01does not show the initial spike exhibited by GF98,and shows a periodicity(5.21±0.05s) consistent with the value measured for the quiescent X-ray source soon after IF01(Woods et al.2003),with no evidence for a glitch like in the case of GF98(Woods et al.1999c). Moreover,it does not show the high-frequency(10–1000Hz) erratic variability which is detected from GF98,although this might be due to lower counting statistics.However the two

14Guidorzi et al.:Large?ares from SGR1900+14with BeppoSAX

?ares show also similar spectral properties.The photon spec-trum of IF01and the corresponding spectrum of GF98dur-ing the?rst40s(corresponding to the time duration of IF01) are both best?t with a three–component(BB+BKNPL+PL) model,with similar BB temperature(～15keV)and break en-ergy(E break～73keV)of the BKNPL model.However,the power-law indices of the BKNPL are different,resulting higher (and the spectrum softer)for IF01.The highest energy sections of the spectra(>300keV)are both well?t with a power-law with marginally similar positive photon indices.This power-law component contributes,in both cases,to～2%of the40–700keV?uence of the two?ares.

In the magnetar model scenario,the entire2001?are and the intermediate stage of GF98(before the pulsation is set up clearly)could be both interpreted as radiation coming from a transient pair-dominated corona surrounding a trapped?reball anchored to the neutron star surface,although other interpreta-tions can be possible.The high-frequency noise,detected dur-ing the intermediate stage of GF98,could directly trace the evo-lution of fractures propagating throughout the neutron star crust soon after the dramatic spike.The PSD of the non–Poissonian noise is in agreement with the expectations of the“Integrate And Fire”(IAF)model(Davidsen&Schuster2002),accord-ing to which,similarly to earthquakes,discrete energy releases occur when a variable threshold is exceeded.

The appearance of a last isolated pulse at the end of IF01 might point to a different origin from what caused the?are:its peculiar time pro?le is similar to that of short bursts from the same source.While the main time pro?le of IF01could have come from the outer layer of the pair corona,the last pulse might have originated close to the surface. Acknowledgements.We thank Sandro Mereghetti for carefully read-ing this manuscript and for his comments.This research is supported by the Italian Space Agency(ASI)and Ministry of University and Scienti?c Research of Italy.We wish to thank the Mission Director L.Salotti and the teams of the BeppoSAX Operation Control Center, Science Operation Center and Scienti?c Data Center for their support. References

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如何写先进个人事迹

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的主体，要下功夫写好，关键是要写得既具体，又不繁琐；既概括，又不抽象；既生动形象，又很实在。总之，就是要写得很有说服力，让人一看便可得出够得上先进的结论。比如，写一位端正党风先进人物的事迹材料，就应当着重写这位同志在发扬党的优良传统和作风方面都有哪些突出的先进事迹，在同不正之风作斗争中有哪些突出的表现。又如，写一位搞改革的先进人物的事迹材料，就应当着力写这位同志是从哪些方面进行改革的，已经取得了哪些突出的成果，特别是改革前后的．经济效益或社会效益都有了哪些明显的变化。在写这些先进事迹时，无论是先进个人还是先进集体的，都应选取那些具有代表性的具体事实来说明。必要时还可运用一些数字，以增强先进事迹材料的说服力。为了使先进事迹的内容眉目清晰、更加条理化，在文字表述上还可分成若干自然段来写，特别是对那些涉及较多方面的先进事迹材料，采取这种写法尤为必要。如果将各方面内容材料都混在一起，是不易写明的。在分段写时，最好在每段之前根据内容标出小标题，或以明确的观点加以概括，使标题或观点与内容浑然一体。最后，是先进事迹材料的署名。一般说，整理先进个人和先进集体的材料，都是以本级组织或上级组织的名义；是代表组织意见的。因此，材料整理完后，应经有关领导同志审定，以相应一级组织正式署名上报。这类材料不宜以个人名义署名。写作典型经验材料-般包括以下几部分： (1)标题。有多种写法，通常是把典型经验高度集中地概括出来，一

《女人的资本》读后感,-女性必读的三十部经典-最新范文

《女人的资本》读后感,:女性必读的三十部经典篇一：女人一生必读的本书女人一生必读的本书世界有十分美丽,但如果没有女人,将失掉七分色彩;女人有十分美丽,但如果远离书籍,将失掉七分内蕴。有人说,书是女人最好的化妆品。做时尚的女性,不需要掌握男人,只需要善待自己。读书的女人是美丽的。正如著名女作家毕淑敏所说：“日子一天一天地走,书要一页一页地读。清风朗月水滴石穿,一年几年一辈子地读下去。书就像微波,从内到外震荡着我们的心,徐徐地加热,精神分子的结构就改变了、成熟了,书的效力就凸现出来了。”女人不可不读书,世界因女人的存在而美丽,女人因书籍的滋养而变得更加聪慧. 1《第二性》被《时代》周刊评为20世纪改变人类思想和生活的10本书之一当代西方女权主义运动的“圣经” 迄今为止对女性问题研究得最为透彻的一本书 2《写给女人》畅销全球的女性缔造成熟之爱、获取人生幸福的经典之作当代女性的必读文本为广大女性朋友们提供了切实可行的人生指导和精神启迪 3《红楼梦》中国古今第一奇书中国古典小说的巅峰之作

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幼儿教育书籍读后感

篇一：卡尔威特的教育读后感作为妈妈和老师，我对儿童教育方面的书籍一直是更为关注一些。一次在新华书店里，发现的这本书。《卡尔·威特的教育》真的是一本好书，这是一本关于幼儿教育方面的书籍，是一部有有着很长的历史的经典教育书籍。因为是教师，所以我带着疑问的眼光读完老卡尔写的育儿经验，卡尔威特在三个世纪前的教育经验在现世仍然具有很大的参考意义。对现代的小学教育，仍有很多地方可以借鉴。素质教育很早就开始有了，至少在卡尔威特的教育方式上就是这样应用的。以素质教育的非智力因素打下基础，在上面建筑一个神童般的宫殿，这就是卡尔威特的成功秘诀。教育孩子要有正确的方法，要培养孩子的生活自理和良好的行为习惯，要开发孩子的智力，引导孩子对周围事物的兴趣，养成勤于思考、善于思考的习惯。培养孩子发现问题、解决问题的能力，要鼓励孩子敢于向成人提问，作为老师和父母，我们可能什么都知道，只要把问题的思考和解决的方法和步骤展现在孩子面前。明确告诉孩子你不懂或不清楚，但可以一起查书，上网或者请专家。在引导孩子查书找资料、向别人请教的过程中，孩子学到的不仅仅是知识，同时培养了孩子对读书的好奇心、发现问题的恒心、解决问题的自信心。要养成孩子的好习惯。专心致志的习惯——学习必须专心致志才能有好的结果。学语文时就只考虑语文，学数学时就专心于数学，如果在学习时想着玩，玩时又担心学习跟不上，不能用心一处，即使学生整天坐在书桌旁，那也只不过是装装样子而已，只是一种对自己和别人的一种欺骗。学习任何学科也是一样，只有专心致志才能学好。敏捷灵巧的习惯——一部分学不拖到最后就不想做，久而久之，这些学生作业一直迟交，甚至不交，其实这些学生不明白，迅速完成作业之后，多余的时间可以做自己喜欢做的事，发展自己的爱好。如果不养成敏捷，灵巧的习惯，能做的事就更少了！坚持不懈的习惯——在学习上会有很多难以预料的困难，但是只要有恒心，只要能够坚持，那么一切困难都会迎刃而解。好习惯是从小养成的，小学阶段是养成好习惯的关键时期，所以我觉得无论是老师还是父母，都应该重视培养孩子良好的习惯。从玩中学是孩子更易接受的，父母要常深入研究。辅导孩子的过程和孩子学习的过程都应是快乐的，并且成效显着的话，我想智慧的大门就打开了。早期教育是非常的重要，不都是说“三岁决定人的一生”吗？但又是什么在三岁之前决定了孩子的一生呢？是早期的识字教育？早期的数学教育？还是早期的才艺教育？这些并非不重要，但却不是最重要的。这本书的副标题为：为孩子的终身学习奠定良好的基础。这让我想起了圣经里的一句话：“凡听见我的话就去行的，好比聪明人，把房子盖在磐石上。雨淋，水冲，风吹，撞着那房子，房子总不倒塌，因为根基立在磐石上。凡听见我的话不去行的，好比一个无知的人，把房子盖在沙土上。雨淋，水冲，风吹，撞着那房子，房子就倒塌，并却倒塌得很大。” 你愿意你的孩子是那磐石上的房子，还是沙土上的呢？我想没有人选择后者，那么这本书会教给你，如何站在孩子的角度，读懂孩子的行为，并将孩子的行为引导到一个有效的目标上去。就像圣经里说的：“教养孩童，走他当行的路，就是到老他也不偏离。”

《俗世奇人》读后感

《俗世奇人》读后感本文是关于读后感的，仅供参考，如果觉得很不错，欢迎点评和分享。《俗世奇人》读后感（一）《俗世奇人》里面的一个个人物，一个个故事讲得都是发生在码头上的。动作干净麻利的苏七块；力大无边的张大力；手巧灵活的泥人张……读了《俗世奇人》这本书后，书中觉得让我最佩服的人是——张大力。一听到这个就觉得他很有力气。他原名叫张金璧，津门一员赴赴武功，身强力蛮，力大无边，所以那里的人都故称他大力。天津人都知道他的名字，他之所以力气大这么多人知道他的名字的原因就是：侯家后有一家石材店，叫聚合成。大门口放一把死沉沉的青石大锁，锁把也是石头做的，锁上刻着一行字：凡举起此锁者，赏银两百。旁观的人不停地嘀咕着，没人举起过，甚至没人能叫它稍稍动一动，您而猜出它有多重吗？一天，张大力到侯家后，看到这把锁，也看到了上边的字，便俯下身子，使手问一问，轻轻一撼，竟然摇动起来，而且赛摇一竹篮子，人们看到了，都赶紧围上来看。只见张大力手握锁把，腰一挺劲，大石锁被他轻易地举到空中胳膊笔直不弯，脸上遍布笑容老板上来笑嘻嘻的说：“张老师，您没看锁下还有一行字吗？”张大力怔了一下，石锁下写着：唯张大力不算！张大力扔了石锁，扬长而去！

我最后的感受是：码头上的人，不强活不成，一强就出生各样空前绝后的人物，但都是俗世奇人；小说里的人，不奇传不成，一奇就演出各种匪夷所思的事情，却全是真人真事！《俗世奇人》读后感（二）《俗世奇人》是着名作家冯骥才创作的同名小说集，也是冯骥才的第一本小说。全书由19个短篇小说连缀构成，各篇文字极精短，本书用天津方言以及古典小说的白描入笔，极具有故事性和传奇性，读起来让人拍案叫绝。书中的故事素材均收集于长期流传津门的民间传说，写出生活在天津的诸般奇人妙事。故事生动有趣，惟妙惟肖，使人物跃然纸上，令人赞叹不已。在当时，“天津卫”是天津的古称，它既是水陆交通要道，也是世人瞩目的开放城市。所以，在天津生活的人，“不强活不成，一强就生出各样空前绝后的人物”。他们有的现身于上流社会，有的混迹在市井民间，都是“俗世”中人；然而他们又不是普通人，他们所做的事情令人匪夷所思，是“俗世”中的“奇人”。他们中间有凭着一把钓竿把鱼钓绝的大回；有看病前必先收七块银洋的正骨医生“苏七块”；既有专会溜须拍马的“死鸟”贺道台，也有造假画的黄三爷以假乱真耍得蓝眼丢了饭碗。书中粉刷匠“刷子李”干完活全身不沾一个白点；泥人张从鞋底上取下一块泥巴便单手捏出活人嘴脸……皆是些听起来神乎其神，实际上存在过的人物。这些“俗世奇人”，在作家冯骥才独到的眼里、幽默的笔下，个个生动有趣，活灵活现。

经典教育类书籍读后感

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远，无法感受生命开始的神圣，也无法感受死亡宣判的恐惧。我们只是在行走，一路寻找一路走，“生”在脚下延续，“意义”可能在心里，可能在脚印里，始终遍寻不见。但我始终相信，有自我感知，有精神品级，就足够。爱是人生最美的梦，爱情一直是不朽的传说。人类想要幸福，把“爱情”当作终极象征的幸福，但世间好多的爱都不幸福，要么是难成眷属的无奈，要么是终成眷属后的厌倦，就如庄子云，“相濡以沫不如相忘于江湖”。相濡以沫，却让人厌倦到老；相忘于江湖，却让人怀念到哭。爱不是一潭死水，而是一股涓涓细流，时间在走，一切在变。没有什么人什么事会静止不动地等在原地。拥有的时候要懂得珍惜，失去的时候要懂得忘记，再铭记于心的曾经也只是过去，过去在去。回忆始终是时光赠予的最好的礼物，带着这份礼物，可以微笑着往前走。爱与孤独一直是个矛盾，人怕孤独，这是大多数人的宿命。宿命的原因在于他们不理解孤独，孤独源于爱，无爱的人不会孤独，理解孤独的人学会珍惜自己，能领悟人生根本性孤独的人，便已经站到了一切人间欢爱的上方，不会做爱的奴隶，不会丢失自己。对人生深刻的感受大多是自我意识的产物，很难让别人懂你所懂，想你所想。所以，学会孤独，学会与自己交谈，听自己说话，就这样学会深刻。无聊者自厌，寂寞者自怜，孤独者自知。理解孤独的人，内心会冷暖自知，会眼神清亮，是一种智慧。 “人生唯一能够追问自身存在具有什么意义的生物，这就算人的伟大之处，但也正是人的悲壮之处，因为对自己的存在意义没有明确的标准。”人寻求生命存在的意义，其实可贵的并不在于意义本身，而是在于寻求的过程！生或死，

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与孩子一起成长读后感与孩子一起成长读后感（一）儿女的成长只有一次，与他们一起成长，是责任，是幸福，也是一门艺术。厚厚的一本书翻完，作者对女儿的一片爱心跃然纸上，本书是作者送给女儿的一份生日礼物，也是作者对自己培养孩子全过程的一个系统总结，李镇西老师既是一个学校的教育者，又是一位家庭教育者，视野全面客观，不存在厚此薄彼，以偏盖全之说，正适合当下有心于教育孩子的既是教师，又是家长的我们阅读。作者从日常生活中的一点一滴，一事一物入手，阐述了教育其实并不高深，寻常处，见真谛。书中，李镇西老师告诉我们“家长也是教育者”，“教”“育”是相辅相成的，在我们教育子女的同时子女也在教育着我们，而且家庭教育和学校教育应该是和-谐的统一，作为家长首先应该是一位当之无愧的教育者，是孩子永远的老师，无论是学校老师或家长，其教育的目的都是为了把孩子培养成优秀的可造之才。我从未认为教育孩子只是学校老师的事情，也从不认为把孩子送到学校自己就完全放心，万事大吉。但在实际行动中却在这样做，读完本书后自觉惭愧。李镇西老师记录女儿生命成长的历程，是用心在记录。从女儿一颦一笑到女儿许多的第一次，无不体现了一位伟大父亲对女儿的记挂和关爱。第一次随爸爸妈妈坐公交车，第一次呈现出笑的表情，第一

次独坐，第一次“手足舞蹈”地跳舞……无不体现出伟大的爱心。十八年，父亲从年轻到中年，从女儿呀呀学语到幼儿园到小学到初中到高中到亭亭玉立的大学生，失败则鼓励，迷惘则开导，困惑则解惑，始终充满期待充满微笑。李老师在书中强调：“和许多年轻的父母一样，我非常爱我的女儿，但我不把我曾有过的‘科学家梦’、‘艺术家梦’强加给她。我抱定一个信念：我要让她成为一个快乐的人！而什么是快乐呢？李镇西告诉女儿：”快乐，源于善良：让人们因我的存在感到幸福，就是最大的快乐！快乐，源于知识：畅游在浩瀚知识的无边海洋，就是最大的快乐！快乐，源于童心：永远保持赤子般的纯净无暇，就是最大的快乐！快乐，源于超越：战胜自己并争取做最好的自己，就是最大的快乐！原来，快乐就是如此朴实的一个概念。是的，世界上的孩子千差万别，不同的家庭，不同的环境，自然有着不同的孩子。这些孩子不一定智慧超常、才高八斗，不一定都能成名成家，铸成大器，不可能样样优秀，处处超越别人。但是，不论怎样的孩子，我们应该把他们培养成善良和快乐的人，塑造孩子完整的人格，让他们拥有一个幸福的人生。所以，“让女儿成为一个快乐的人！和女儿一起快乐地成长！”是李镇西坚定不移的家庭教育理念，也应该成为我们教育子女坚定不移的理念。翻看多遍后，才发觉何谓“最好”？只有对比才有好坏，而此中的“最好”，却不是让家长们之间互相比较出来的“最好”，而是家长

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俗世奇人读后感作文五篇俗世奇人读后感作文篇一：《俗世奇人》这本书讲的是在平凡的世间生活着各式各样的、独一无二的的本领的人，在当时那算得上是赫赫有名。他们每人只要有独一无二的绝技或者是另有绝活的，那就一定有绰号，比如说：像刷子李、刻砖刘、泥人张、风筝魏、机器王、苏金散等等。津门人好把这种人的性，和他拿手擅长的行当连在一起称呼。时间一长，名字不知道，倒知道一个响当当的绰号。在刚看这本书的第一章《苏七块》时，我就一直在想：难道这本书里的这些人都有自己先天的能力？最让我感动的是：刷子李和苏金散，刷子李他刷完之后就绝不会有一个白颜色的小点；苏金散凭着他精湛的医技赢得了民众的尊敬。读完了这本《俗世奇人》我才知道这是怎么一回事原来我们一个个生下来并不是天才，而是靠后天付出“百分之九十九的努力，和百分之一的汗水。” 这不正体现出我可爱而又宽松的生活中的一个例子吗？在我刚开始学习舞蹈平转的时候我练了不到五分钟，我就不耐烦了，我觉得肯定练不好了，妈妈并没有逼着我练，而是在在网上查了一个有关平转的杂技表演拉出来给我看有句俗话说的好：台上一分钟，台下十年功。我想：她们居然能在舞台上表演杂技而且还是我连不好的平转。于是我信心十足的开始练平转，一遍练不好，练第二遍；第二遍练不好，练第三遍；三遍练不好练第四遍……我练了十遍终于练成了平转。

让我们在赛道上赛跑，即使摔倒了，不要气馁也不要懈怠，爬起来继续跑。俗世奇人读后感作文篇二：生活是平凡的，但不是平淡的。平凡的生活中同样也是波澜起伏，妙趣横生。冯骥才老师的《俗世奇人》说得好，“手艺人靠的是手，手上就必得有绝活”，“各行各业，全有几个本领齐天的活神仙。刻砖刘、泥人张、风筝魏、机器王、刷子李等等。天津人好把这种人的姓，和他们拿手擅长的行当连在一起称呼。叫长了，名字反没人知道。只有这一个绰号，在码头上响当当和当当响。” 在平凡的生活中，这些有“绝技”的奇人，生活会平淡吗？但问题的关键在于，“手艺人靠的是手，手上就必得有绝活。有绝活的，吃荤，亮堂，站在大街中央；没能耐的，吃素，发蔫，靠边呆。这一套可不是谁家定的，它地地道道是码头上的一种活法。” 得有真本事，才不会平淡啊！没有真本事，岂只平凡、平淡，还会更加糟糕，把生活过得一塌糊涂。我们要把平凡的生活过得不平淡。就得靠那份才艺，不只是在那时候这套是种活法，就今时今日才华也是人不可缺少的啊。在这时代有才华的人不怕遇不上伯乐，只怕才华比不上别人。随着社会的进步，物尽天择，强者生存，弱者淘汰，这不算残酷，这只是一个事实而已。《俗世奇人》中的奇人并不是样样精通，但他们却把生活过得有滋有味，受人尊敬，当今社会也是一样，我们不可能成为面面俱到

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