The neutron star in the supernova remnant PKS 1209–52. Astron. Astrophys

The neutron star in the supernova remnant PKS 1209–52. Astron. Astrophys
The neutron star in the supernova remnant PKS 1209–52. Astron. Astrophys

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ASTRONOMY

AND ASTROPHYSICS

30.9.1997

The Neutron Star in the Supernova Remnant PKS1209–52

V.E.Zavlin1,2,G.G.Pavlov2and J.Tr¨u mper1

1Max-Planck-Institut f¨u r Extraterrestrische Physik,D-85740Garching,Germany

2The Pennsylvania State University,525Davey Lab,University Park,PA16802,USA

September30,1997

Abstract.We re-analyzed soft X-ray data collected with the ROSAT and ASCA observatories on a candidate neutron star(NS)near the center of the supernova remnant PKS1209–52.We?tted the observed spectra with NS atmosphere models.The hydrogen atmosphere?ts yield more realistic parameters of the NS and the intervening hydrogen column than the traditional blackbody?t.In particular,for a NS of mass1.4M and radius10km,we obtained the NS surface temperature T e?=(1.4?1.9)×106K and distance d=1.6?3.3kpc versus T=(4.2?4.6)×106K and(implausible) d=11?13kpc for the blackbody?t,at a90%con?dence level.Our?ts suggest that the surface magnetic?eld is either very weak,B<~1010G,or it exceeds 2×1012G.The hydrogen column density inferred from the atmosphere?ts, n H=(0.7?2.2)×1021cm?2,agrees fairly well with independent estimates obtained from UV observations of nearby stars,radio data,and X-ray spectrum of the shell of the supernova remnant,whereas the blackbody and power-law ?ts give considerably lower and greater values,n H=(0.2?0.4)×1021and(5.2?7.0)×1021cm?2,respectively.The inferred NS surface temperature is consistent with standard NS cooling models.

Key words:stars:neutron:individual(1E1207.4–5209)—supernova remnants:individual(PKS1209–52)—X-rays: stars

1.Introduction

In addition to about15radio pulsars associated with supernova remnants(Gaensler&Johnston1995),several radio silent isolated neutron star(NS)candidates within SNRs have been observed with the X-ray observatories HEAO A, Einstein,EXOSAT,ROSAT,and ASCA(see Caraveo,Bignami&Tr¨u mper1996for a review).These objects have not been detected outside the X-ray range,and their X-spectra resemble blackbody(BB)spectra with temperatures of a few million kelvins.If they are indeed thermally emitting NSs,the analysis of their radiation provides an opportunity to study thermal evolution of NSs of ages~103?105yr,which is important for elucidating the properties of the superdence matter in NS interiors.

One of the most convincing examples of such objects is the point-like source1E1207.4–5209within the barrel-shaped radio,X-ray,and optical SNR PKS1209–52(also known as G269.5+10.0).From the analysis of radio and optical observations of this SNR,Roger et al.(1988)estimated its age~7000yr,with an uncertainty of a factor of3,and concluded that the remnant is in an adiabatic expansion phase.The distance to PKS1209–52is not well determined—estimates in the range1.1?3.9kpc were suggested(Milne1979;Mills1983).Estimates of the interstellar hydrogen column density from the radio and optical data yield n H,21≡n H/(1021cm?2)~1.0?1.8(see Roger et al.1983and Kellet et al.1987for references),consistent with a distance d~1?2kpc.

After the?rst X-ray detection of PKS1209–52with HEAO A-1(Tuohy et al.1979),the point source1E1207.4–5209was discovered with the Einstein observatory(Helfand&Becker1984),6 o?-center the81 diameter SNR.Matsui, Long&Tuohy(1988)concluded that its spectrum can be interpreted as a BB spectrum with an apparent temperature T=1.4×106K(assuming n H,21=3.2,as obtained from the HEAO A-1observations).The Einstein High Resolution Imager(HRI)observations showed a lack of di?use X-ray emission around1E1207.4–5209(later con?rmed by the ROSAT HRI observations),which greatly simpli?es the analysis of the point source radiation.From the analysis of EXOSAT observations,Kellett et al.(1987)estimated the BB temperature of the central object T=1.8×106K(at

2Zavlin et al.:Neutron Star in PKS1209–52

n H,21=1.1),which implies an emitting area of a radius(3?4)d2km,where d2=d/(2kpc).Applying the Raymond &Smith(1977)line-emission model,Kellet et al.estimated also an average SNR temperature,~1.7×106K,and the hydrogen column towards the SNR,n H,21 1.4,consistent with the values obtained from radio and optical data.

Observations of PKS1209–52and its central source with ROSAT and ASCA have further supported the NS hypothesis for1E1207.4–5209.Mereghetti,Bignami&Caraveo(1996;hereafter MBC96)showed that the ROSAT data on1E1207.4–5209can be interpreted as blackbody emission of T~3×106K from an area with radius R~1.5d2km.

The authors noticed that this temperature is too high to be explained in the framework of a cooling NS with age of PKS1209–52(~104yr).The hydrogen column inferred from the BB?t,n H,21~0.4,is3–4times lower than the estimate given by Kellett et al.(1987).From observations at4.8GHz,MBC96found an upper limit of~0.1mJy on

the radio?ux from1E1207.4–5209.They also set a deep limit of V>25for an optical counterpart in the Einstein HRI error circle,that supports the hypothesis that1E1207.4–5209is indeed an isolated NS.

Vasisht et al.(1997;hereafter Val97)have recently analysed ASCA observations of1E1207.4–5209.They found

that each of the three spectra obtained with the ASCA detectors can be?tted by a BB spectrum consistent with that obtained from the analysis of the ROSAT data.The hydrogen column is poorly restricted in the ASCA spectral?ts due to low detector sensitivities at photon energies https://www.360docs.net/doc/065996746.html,ing a?t with a Raymond-Smith model at?xed cosmic abundances to the ROSAT data on the SNR shell,Val97estimated the remnant temperature~(1.9?2.3)×106K and the foreground column density n H,21~0.6?0.9.They attributed the di?erence in n H between the NS and SNR?ts to either separate lines of sight or the large column density that the shell X-rays can encounter in the SNR postshocked gas.

Based on the results of the blackbody analysis,both MBC96and Val97concluded that1E1207.4–5209is an isolated NS with hot spots on its surface,aligned with the magnetic poles.Val97suggested that the spots are heated either by dissipative heating in the NS interior or by the bombardment of polar caps by relativistic particles from the NS magnetosphere if1E1207.4–5209is an active pulsar.However,the former hypothesis can hardly explain the small sizes of the hot spots,even with allowance for large anisotropy of thermal conductivity of the magnetized NS crust. The latter heating mechanism is also in doubt because of the absence of radio andγ-ray emission from1E1207.4–5209. Moreover,both the ROSAT and ASCA data did not reveal pulsations,which may not be consistent with the presence of the hot spots unless the magnetic and rotation axes are coaligned.

Although it looks very plausible that1E1207.4–5209is a thermally emitting isolated NS,the BB interpretation adopted by previous authors leaves several controvertible points.On the other hand,thermal radiation emitted by NS atmospheres may signi?cantly di?er from the BB radiation.Therefore,to resolve the inconsistencies following from the simpli?ed BB interpretation,it is natural to employ more realistic models of NS radiation.Here we present a combined analysis of the ROSAT and ASCA data based on NS atmosphere models(Pavlov et al.1995,and references therein).These models have been applied successfully to the interpretation of the soft X-ray radiation from,e.g., the Vela pulsar(Page,Shibanov&Zavlin1996)and the brightest millisecond pulsar J0437–4715(Zavlin&Pavlov 1997;Pavlov&Zavlin1997).These examples show that?tting the soft X-ray pulsar spectra with hydrogen or helium atmosphere models always results in lower e?ective temperatures and greater emitting areas(or smaller distances) than those obtained from the BB?ts.

We show in§2that,indeed,the model atmosphere?ts of the X-ray radiation from1E1207.4–5209yield an NS

surface temperature compatible with NS cooling models,and they do not require hot spots on the NS surface.Moreover, the hydrogen column density inferred from this interpretation is in excellent agreement with that obtained from our ?ts of the SNR X-ray radiation as well as with independent estimates of n H for stars in the vicinity of1E1207.4–5209 (§3).These results warrant application of the same approach to other similar objects and enable one to obtain reliable estimates of surface temperatures of NSs of di?erent ages.

2.Observations and results

We used archival ROSAT and ASCA data on1E1207.4–5209(see MBC96and Val97for a detailed description). Four ROSAT Position Sensitive Proportional Counter(PSPC)pointings(obtained in1993July,with exposure times ≈5?6ks each—see Table2in MBC96)were centered at di?erent positions(o?-axis angles between16 and33 ).We checked that the spectra of1E1207.4–5209extracted from each of the four data sets and properly corrected for the PSPC response are consistent with each other.For the combined analysis with the ASCA data we chose the ROSAT PSPC observation with the minimum o?-axis angle16 (exposure time4.97ks).We extracted a raw spectrum from a region with a radius r 75 centered on the source.The(o?-axis)source count rate is0.145±0.005s?1.We binned this spectrum into24spectral bins in the0.1–2.4keV energy range for further analysis.The ROSAT HRI counts for each of the three on-axis pointings(obtained in1992August and1994July;total exposure time≈14.5ks)were

Zavlin et al.:Neutron Star in PKS1209–523 selected from the circles of r 22 .The corresponding source count rate is0.064±0.003s?1,in agreement with MBC96.

The ASCA data were obtained in1994July,with two Solid State Imaging Spectrometers,SIS0and SIS1,in the bright mode,and two Gas Scintillation Imaging Spectrometers,GIS2and GIS3,in the pulse-height mode.The SIS1 image of1E1207.4–5209is too close to the edge of the CCD chip for a reliable spectral analysis.The SIS0source counts collected in≈21ks(with high and medium bit rates)were extracted from the circle of r 4 ,the total source count rate is0.0556±0.0017s?1.The SIS0spectrum was binned into38spectral bins in the0.5?10.0keV range.The GIS2and GIS3counts were extracted from circles of r 9 (exposure≈19ks for the high plus medium bit rates). The source count rates are0.0425±0.0018(GIS2)and0.0533±0.0025s?1(GIS3).The spectra were binned into40 and45spectral bins in the0.3?5.0keV range for GIS2and GIS3,respectively.The total source count rates for all the three ASCA instruments are somewhat lower than those reported by Val97,perhaps because of di?erent screening criteria we applied.

As a?rst step of our data analysis,we?tted the count rate spectra simultaneously for the four instruments, ROSAT PSPC and ASCA SIS0,GIS2,and GIS3,with the traditional power-law and BB models.Figure1shows the results of these?ttings.The power-law?t yields a photon indexγ=5.2(+0.4,?0.3)and a hydrogen column density,n H,21=6.0(+1.0,?0.8)(minimumχ2ν=1.47,ν=144;the uncertainties hereafter are at a90%con?dence level).These values ofγand n H are better constrained than those obtained by MBC96from the PSPC data alone,γ=3.9(+1.5,?1.4)and n H,21=3.0(+2.5,?1.8)(minimumχ2ν=1.61,ν=10).The photon index is unusually large in comparison with typical values,γ~1.5?2.5,observed from,e.g.,X-ray emitting radio pulsars(Becker& Tr¨u mper1997),and the hydrogen column density too much exceeds the values obtained by independent measurements (see below).These discrepancies,together with the too high minimumχ2ν,imply that the power-law interpretation is inadequate.

The BB temperature(as measured by a distant observer),T∞=3.12(+0.15,?0.11)×106K,the apparent radius

of the emitting area,R a=1.21(+0.10,?0.13)d2km,and the bolometric luminosity,L∞

bol =0.93(+0.19,?0.11)×

1033d22erg s?1,obtained from the combined?tting(Fig.1)are very close to the values from the separate?ts of

the ROSAT and ASCA data by MBC96and Val97.The hydrogen column density in the combined?tting,n H,21=

0.28(+0.15,?0.12),is compatible with(albeit slightly lower than)the value of n H,21=0.3?0.5inferred from the separate ROSAT PSPC spectrum.Although the quality of the BB?t is better than of the power law?t,the n H

values look surprisingly low in comparison with(1.0?1.8)×1021cm?2obtained from independent estimates(see

Introduction).

Since thermal NS spectra,as well as spectra of ordinary stars,cannot exactly coincide with the BB spectra because

of the e?ects of radiative transfer in the emitting layers,it is natural to compare them with more realistic model

spectra of NS atmospheres(e.g.,Pavlov et al.1995).Strongest deviations from the BB spectrum are expected if the NS surface is covered with a hydrogen atmosphere.Hydrogen may appear at the NS surface as a result of,e.g.,

accretion of interstellar matter or post-supernova accretion of a fraction of the ejected envelope.Due to the huge

surface gravity(typical gravitational acceleration~1014?1015cm s?2),heavier chemical elements sink down in deeper layers and do not a?ect properties of emitted radiation,whereas hydrogen remains at the surface.The shape

of the spectrum emitted by an atmosphere depends on the strength B of the NS surface magnetic?eld.The lack of pulsations does not allow one to estimate B using period and its derivative,as is usually done for pulsars.The absence of statistically reliable features in the observed spectra,which could be associated with an electron cyclotron line at E Be=11.6(B/1012G)keV,prevents one to make a direct estimation of B.Therefore,one has to try the atmosphere models with both low(B<~1010G)and high magnetic?elds.(In the former case,the?eld does not a?ect properties of emergent radiation[Zavlin,Pavlov&Shibanov1996],so that we can merely put B=0).In the case of strong nonuniform?eld(B>~1012G),the NS should have a nonuniform temperature distribution along its surface because of the high anisotropic thermal conductivity in the NS crust(e.g.,Shibanov&Yakovlev1996).However,since we have no information about the?eld geometry,we assume that the magnetic?eld has the same strength and is directed radially everywhere at the surface,and the e?ective temperature is uniform.This assumption reduces the number of ?tting parameters and can be considered as a reasonable?rst approximation for investigating the atmosphere e?ects.

Figure2shows results of?tting of the combined ROSAT and ASCA data with hydrogen atmosphere models

for three?xed values of the magnetic?eld.In these?ts we assume canonical values for the NS mass and radius, M=1.4M and R=10km,and consider the distance as a?tting parameter.The models with B=0(left panels) and1013G(right panels)result in close values of the distance,e?ective temperature at the NS surface and bolometric luminosity,d=2.3(+1.0,?0.7)kpc,T e?=1.63(+0.27,?0.19)×106K,L bol=5.0(+4.3,?1.8)×1033erg s?1,and d=2.3(+1.0,?0.8)kpc,T e?=1.65(+0.20,?0.17)×106K,L bol=5.3(+3.0,?2.0)×1033erg s?1,for B=0and 1013G,respectively.Since the nonmagnetic spectra are softer at lower energies,the hydrogen column density at B=0,n H,21=1.0(+0.5,?0.6),is lower than for the strong magnetic?eld,n H,21=1.5(+0.7,?0.6).We checked that

4Zavlin et al.:Neutron Star in PKS1209–52

folding the models within the90%con?dence region with the ROSAT HRI response yields count rates compatible with those observed.When the?eld strength varies in the range5×1012<~B<~5×1013G,the?tting parameters remain approximately the same because the model spectra are almost insensitive to the B value in the corresponding domain of energies and e?ective temperatures.When B exceeds~5×1013G,the proton cyclotron line centered at E Bp=0.063(B/1013G)keV(cf.Bezchastnov et al.1996)enters the SIS energy range,which makes the?ts statistically unacceptable.(This line moves above~5keV,a maximum energy where the NS?ux is still above the background, at superstrong magnetic?elds,B>~8×1014G,for which the models we used here are not directly applicable.)When B falls below 5×1012G,the low-energy wing of the electron cyclotron line gets into the ASCA range,and the model spectra become softer at E>~2keV.As a result,the con?dence contours in the n H–d and n H–T e?planes move to greater d and T e?,and lower n H,towards the BB contours.An example is shown in the middle panels of Fig.2for B=2×1012G,for which the best-?t distance is about50%larger than at B=1013G.When the?eld is lower than ~5×1011G,but greater than~1×1010G,the atmosphere model?ts become statistically unacceptable because the core of the electron cyclotron line gets into the ASCA/ROSAT range.

The atmosphere models depend not only on B,but also on the NS mass and radius which determine the gravitational acceleration(one of our model parameters)and the gravitational redshift factor g r=(1?0.295M?/R10)1/2,where M?=M/M ,R10=R/10km.To illustrate this e?ect,we present in Fig.3the best-?t parameters at B=1013G in a wide range of R and M allowed by equations of state of the NS matter.Although the e?ective temperature at the NS surface,T e?,varies by about±20%in the allowed R-M domain,the apparent e?ective temperature(as measured by

a distant observer),T∞

e?=g r T e?,remains almost constant,(1.23?1.31)×106K,because the redshift is compensated

by the change of the unredshifted NS spectrum(it softens in the Wien tail with increasing M and decreasing R at

given T e?).Owing to the approximate constancy of T∞

e?,the apparent and“true”bolometric luminosities depend on

R and M as L∞

bol ∝R2∞=R2/g2r and L bol=g?2r L∞bol∝R2/g4r.The latter dependence explains the non-monotonous

behaviour of L bol at higher M.The best-?t d and n H are almost independent of M at higher R,when g r is close to

1.At lower R the variations are stronger,albeit within the statistical uncertainties of these parameters(cf.Fig.2).

The distance inferred at assumed R and M can be approximately described,in the allowed mass–radius domain,by a linear equation:d=0.5M??0.4+(2.5?0.3M?)R10(in kpc);it grows with R faster than for the BB interpretation. Notice that if d is determined more accurately in future observations of the SNR and its central source,this equation

would delimit a band in the M–R plane constraining equation of state of the NS matter.

Since the hydrogen atmosphere?ts yield n H greater than the BB?t by a factor of3–5,it is important to estimate this parameter independently.For this purpose,we?tted the SNR emission with various models for thermal plasma radiation.We extracted the SNR spectrum from a bright region of the ROSAT PSPC image of the remnant shell within the r 5 circle centered atα(2000)=12h11m56.s0,δ(2000)=?52?36 36 .Three models available with the XSPEC package,vraymond,vmeka,and vmekal(Raymond–Smith,Mewe–Gronenschild–Kaastra,and Mewe–Kaastra–Liedahl models with variable abundances)give satisfactory?ts(χ2ν<1.0)with the column density to the SNR in the range of (1.1?1.9)×1021cm?2,consistent with the hydrogen atmosphere?ts of1E1207.4–5209,but certainly in excess of the BB?ts.The inferred plasma temperature is(1.9?2.1)×106K.These results were obtained with a moderate excess of abundances of Al and Si whose emission lines are prominent in the SIS spectra of the SNR shell.Abundances of other elements are close to standard values.The SNR parameters inferred from our?ttings are consistent with those obtained by Kellett et al.(1987)from the EXOSAT data.The lower hydrogen density,n H,21=0.6?0.9,obtained by Val97,is likely associated with?xed cosmic abundances adopted,that resulted in lower statistical quality of their?ts (χ2ν=1.8).

3.Discussion and conclusions

We have shown that the X-ray spectra of the isolated NS1E1207.4–5209in the center of the SNR PKS1209–52 observed with the ROSAT PSPC and HRI and ASCA SIS0,GIS2and GIS3can be interpreted as thermal radiation from the hydrogen-covered,uniformly heated surface of the NS.The proposed interpretation resolves all the inconsistencies which follow from the BB interpretation of radiation of this object.

First,the range of distances,d=1.5?3.2kpc,inferred for the standard NS mass M=1.4M and radius R=10km,is within the(conservative)limits,1.1?3.9kpc,obtained from radio observations of the SNR.This range shifts to lower distances with decreasing R and M:e.g.,d=1.2?2.6kpc for M=1.0M ,R=8km.Thus, the assumption about hot spots on the NS surface,which is di?cult to reconcile with the lack of pulsar activity in 1E1207.4–5209,is super?uous in our model.

Second,the e?ective temperature T e?=(1.4?1.9)×106K(T∞

e?=(1.0?1.6)×106K),obtained from the?ttings

with our hydrogen atmosphere models,matches well to a number of the NS cooling models(see Fig.4and discussion below).On the contrary,it is di?cult to reconcile the results of the BB interpretation with models of the NS cooling.

Zavlin et al.:Neutron Star in PKS1209–525 Third,the inferred hydrogen column density towards the1E1207.4–5209,n H,21=0.9?2.2and0.5?1.5for high and low surface magnetic?elds,respectively,agrees fairly well with n H,21=1.1?1.9obtained from?tting the spectra of the SNR shell.These estimates are consistent with the n H values obtained by Kellett et al.(1987)from the EXOSAT observations of PKS1209–52.Moreover,measurements of n H in UV observations of several stars in the vicinity of1E1207.4–5209(l=296.5?,b=9.9?)yield the hydrogen columns in virtually the same range(Fruscione et al.1994):n H,21=1.1?1.5for HD112244(l=303.6?,b=6.0?,d=1.85kps),n H,21=1.4for HD115842(l=307.1?, b=6.8?,d=1.87kps)and HD111822(l=303.1?,b=10.2?,d=2.53kps).On the contrary,the BB?t gives n H,21=0.15?0.45,clearly incompatible with all the other independent estimates.

The fact that1E1207.4–5209shows no pulsar activity can be explained,in addition to the trivial explanation of unfavorable orientation of its magnetic and rotational axes,by slow rotation or/and low magnetic?eld of the NS,so that it falls below the“death line”on the P–˙P diagram,˙P/P3=2×10?17s?3.For the simplest model of the magnetic dipole radiator,the pulsar period increases with time t as P=(P20+2t0t)1/2,where t0=(8π2/3)(B2R6/Ic3)= 0.97×10?13B213R610I?1

45

s,I=1045I45g cm2is the moment of inertia of the NS and B13=B/(1013G).The condition

that the NS is below the death line can be written as t0/P4<2×10?17s?3,or P>8.4B1/2

13R3/2

10

I?1/4

45

s.Hence,if

B is in the range of strong magnetic?elds allowed by our?tting,0.2<~B13<~8,we may expect that the NS rotates slowly,P>~1?2s.If faster pulsations are discovered in future X-ray observations of1E1207.4–5209,it would indicate that B is in the other range compatible with our?ts:B<~1010G.It is worth noting that if the NS was born as a pulsar at an appreciable distance from the death line,only an enormous magnetic?eld,B>~5×1015G at standard NS parameters,could decelerate its rotation so that the pulsar would“die”at the relatively young age,t~104yr.Hence, discovery of slow pulsations would mean that the NS was born slowly rotating unless its magnetic?eld is superstrong.

Since we have estimated the e?ective temperature of the NS,it is interesting to compare it with what is predicted by various cooling models.Figure4shows examples of NS cooling curves from Van Riper,Link&Epstein(1995)for three equations of state(EOS),sti?(Pandharipande–Smith[PS]),intermediate(Friedman–Pandharipande[FP])and soft(Baym–Pethick–Sutherland[BPS]),and two interior compositions resulting in slow and fast cooling(solid and dashed lines,respectively).Cooling curves without additional heating are depicted by thick lines,whereas thin lines show cooling curves for two models,proposed by Epstein&Baym(EB)and Alpar,Cheng&Pines(ACP),for pinning of the super?uid vortices to the crust lattice.They correspond to strong and weak frictional heating associated with the dissipation of energy of di?erential rotation between the NS crust and super?uid interior(only the EB model is available for the BPS EOS).In the same picture we plot boxes corresponding to the inferred atmosphere and BB temperatures of1E1207.4–5209,assuming its age in the range(0.3?2)×104yr,and similar boxes for the Vela pulsar whose X-ray radiation was investigated in terms of the hydrogen atmosphere models by Page et al.(1996).(We adopted (1?4)×104yr for the Vela age,between the conventional characteristic age P/2˙P and an upper limit estimated by Lyne et al.1996).We see that the BB temperature of1E1207.4–5209is well above the values predicted by all these cooling models,whereas the BB temperature of the Vela pulsar is compatible only with the standard(slow)cooling model supplemented by strong heating for the sti?EOS.The e?ective temperature of1E1207.4–5209obtained with the atmosphere?ts is compatible,given the poorly known age,with the slow cooling models for all the three EOS,at moderate or no heating.For the sti?EOS,it is also compatible with the fast(quark)cooling accompanied by strong frictional heating.However,the large NS radius for this EOS would mean a distance d 2.5?5.2kpc(cf.Fig.3), uncomfortably large in comparison with conventional estimates.The same cooling curve(fast cooling with the EB heating for the sti?EOS)is the only one which goes through both the1E1207.4–5209and Vela pulsar boxes obtained from the atmosphere?ts.This,however,does not necessarily mean that slow cooling models or other EOS or other heating rates are excluded.First,the ROSAT PSPC spectrum of the Vela pulsar,used in both BB and atmosphere ?ts,was not observed directly because the pulsar was not resolved from a surrounding mini-nebula of2 diameter, which makes the results of the spectral?ts less certain.Second,one cannot exclude,in principle,that the NS of the Vela pulsar di?ers from1E1207.4–5209(e.g.,the mass of the former may be greater,that could lead to an“exotic”interior composition associated with an enhanced neutrino luminosity and accelerated cooling).Finally,there exist many more cooling models than shown in Fig.4,and some of them may satisfy both the1E1207.4–5209and Vela pulsar temperatures.For instance,a strong neutrino emission induced by the nucleon Cooper pair formation process (see Page1997,and references therein),which was neglected in most of the previous NS cooling models,may result in great variety of cooling curves,depending on the(unknown)parameters of the nucleon pairing(Yakovlev1997). For a more detailed comparison of the inferred temperatures with the cooling models,it would be very important to evaluate more accurately the distance to PKS1209–52(which would constrain the NS radius and hence the EOS)and the age of this object.

There exist a number of other radio silent isolated NS candidates whose observational manifestations are similar to those of1E1207.4–5209.The most convincing example is1E/RXJ0820–4247in the SNR Puppis A,whose BB

6Zavlin et al.:Neutron Star in PKS1209–52

temperature,≈3×106K,and radius,≈2km(Petre,Becker&Winkler1996),virtually coincide with those of

1E1207.4–5209.Another example with similar properties is RXJ0002+6246in the SNR G117.7+0.6(Hailey&Craig

1995),whose identi?cation is,however,less certain because of its faintness(likely,due to a larger distance and greater n H).We expect that applying the NS atmosphere models to the analysis of such objects will allow us to evaluate their

radii and e?ective temperatures,and to constrain their magnetic?elds.

One more radio silent NS candidate,1E1613–5055in the center of the SNR RCW103(Tuohy&Garmire1980), appears as a di?erent kind of object—the BB?tting of its spectrum yields a considerably higher temperature,~7×106K,at a few times smaller radius of the emitting region(Gotthelf et al.1997).However,this object is deeply immersed in the remnant di?use emission so that it is hard to separate its spectrum from that of the SNR,with the

limitied spatial resolution of ASCA.We expect that the forthcoming AXAF and XMM missions would resolve the

point source and provide its spectrum suitable for the detailed analysis.

Acknowledgements.The data were reduced and analyzed with MIDAS/EXSAS,FTOOLS/XSELECT and XSPEC software

packages.We are grateful to Ken Van Riper for providing us with the cooling curves in numerical form,to Dima Yakovlev for

clarifying various aspects of the NS cooling,and to Gordon Garmire for the discussion of X-ray observations of isolated NSs

in SNRs.The work was partially supported through NASA grant NAG5-2807,INTAS grant94-3834and DFG-RBRF grant

96-02-00177G.VEZ thanks the Pennsylvania State University for hospitality and acknowledges the Max-Planck fellowship. References

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Figures

Fig.168%,90%and99%con?dence contours for the power-law and blackbody?ttings to the ROSAT PSPC and ASCA SIS0,GIS2and GIS3spectra of1E1207.4–5209.The lines in the right panel correspond to constant values of radius of emitting area at a distance d=2kpc.

Fig.268%,90%and99%con?dence contours for the NS hydrogen atmosphere?ttings for M=1.4M ,R=10km,and three values of the surface magnetic?eld B to the combined ROSAT and ASCA data.

Fig.3Dependences of the best-?t parameters for the atmosphere?ttings on NS radius R at di?erent values of the NS mass, M/M =0.8,1.0,...2.0.The thick dashed lines delimit the ranges of the apparent temperature and luminosity(upper and lower dashed curves correspond to M/M =2.0and0.8,respectively).

Fig.4Comparison of the surface temperatures inferred from the BB(empty boxes)and hydrogen atmosphere(hatched boxes)?ttings of the spectra of1E1207.4–5209and the Vela pulsar with NS cooling curves for three EOS of the NS matter, two NS compositions,and di?erent models for additional frictional heating.The cooling curves are taken from Van Riper et al.(1995),where more detailed explanations can be found.

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上外小升初面试往届真题 (一) 一、快听快答 (1.2题忘记了!不过是不能准备的,都是生活里的之类的) 3. He left his umbrella here again. (用完整的感叹句回答) 答案:How careless he is! ; What a careless man! 之类的 4. 先是一个女的读5个单词,第二遍一个男的读四个单词,问男的漏读了哪个词? 第一遍:computer, number, picture, 后面两个忘记了 第二遍:(漏读了picture) 5. 听几个单词,思考属于哪一个种类,再举两个例子 Tokyo, Paris (应该还有一个词,也是首都) 举例:首都就可以了(没提到过的) 二、模仿(单词、词组、句子各读两遍) 两个单词我也不认识,只管模仿 句子是英语,挺短的,最多十个词语,像谚语、俗语这种似的 三、听短文,填空(短文读两遍) 这是一篇关于撒哈拉大沙漠的,没记错的话小科学家上有,我背过的,不过有较大的删减改动的 The Biggest Desert The Sahara is one of the world's biggest desert. It covers a substantial part of northern Africa and includes parts of eleven different countries. Many people think that it has always been a desert, but they are mistaken. At one time the Sahara was under water, and them the water went away and plants grew. However, hot winds made everything very dry and then nothing could grow. During the day the Sahara can be the hottest place in the world. One day in 1924, it was 136.4F° or 58C°! At night it is not so hot and in winter it can be very cold. Not many big animals can live in the desert because there is insufficient water. But camels can survive for as long as seventeen days without water. There are also people living in the desert who are called Bedouins. They are nomads, which means that they do not live in the same place all the time, but move about from place to place. 四、看一篇阅读(能准备的),回答问题 关于三个人就一个小女孩 1.朗读短文(读到一半就让你停了) 2.找出表现Wise Head聪明的句子 3.忘了 4. 回答三个听到的问题(不能看卷子) 五、看一首儿歌,想像说话

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