Modeling CHANDRA Low Energy Transmission Grating Spectrometer Observations of Classical Novae with PHOENIX A. Petz∗, P. H. Hauschildt∗, J. U. Ness† and S. Starrfield∗∗ 5 ∗HamburgerSternwarte,Gojenbergsweg112,21029Hamburg,Germany; 0 [apetz,phauschildt]@hs.uni-hamburg.de 0 2 †OxfordUniversity,TheoreticalPhysics,1KebleRoad,Oxford,OX13NP,UK; [email protected] n ∗∗DeptofPhysicsandAstronomy,ASU,P.O.Box871504,Tempe,AZ85287-1504; a sumner.starrfi[email protected] J 5 Abstract. We use the PHOENIX code package to model the X–ray spectrum of Nova V4743 1 Sagittariiobservedwith the LETGSonboardthe Chandrasatellite on 19March2003.To analyze v nova atmospheres and related systems with an underlying nuclear burning envelope at X–ray 2 wavelengths,itwasnecessarytoupdatethecodewithnewmicrophysics.Wedemonstratethatthe 7 X–ray emission is dominatedby thermalbremsstrahlungand that the hard X–raysare dominated 0 byFeandNabsorption.Preliminarymodelsarecalculatedassumingsolarabundances.Itisshown 1 0 thatthemodelscanbeusedtodetermineelementabundancesinthenovaejectabyincreasingthe 5 absorptionintheshell. 0 Keywords: Stellaratmospheres,Novae,CHANDRA,V4743Sgr / h PACS: 97.10.Ex p - o r INTRODUCTION t s a We have modeled X–ray spectra of classical novae (CNe) with the PHOENIX–code : v version 13 [1]. With our models it is possible to determine the effective temperature i X ofthenovaatmosphereandtheformationofX–rayemissioninthenovashell.Weshow r thatit is possibleto determinetheabundances oftheejecta by modellingX–ray spectra a ofCNe and presentourfirst resultsfortheabundancesofC, N,and O. For the comparison of our model with observations we use an X–ray spectrum of NovaV4743Sagittarii(Sgr)observedwiththeLETGSonboardtheChandrasatellitein March2003 [2]. MODELING NOVA ATMOSPHERES IN X–RAYS WITH PHOENIX Our model atmospheres are 1D spherical symetric, expanding, and time independent. The radiative equilibrium is solved in the comoving frame and the radiative transfer is treatedasspecialrelativisticforanatmosphereinfullNLTEwithlineblanketingof8534 atomiclevels from H, He, C, N, O, Ne, Mg, and Fe. We use an exponential density law (r (r)(cid:181) r−n)withagradientofn=3andastandardvelocityfield(v(r)=M˙/4p r2r (r), M˙ = const)withan outervelocityofv =2500kms−1. out The earlier versions of PHOENIX used atomic data from CHIANTI Version 3 (CHI- ANTI3) and the line lists of Kurucz. For this work, we have implemented two new atomic databases, CHIANTI Version 4 (CHIANTI4) [3] and APED1, because the old databases did not provide enough data for the X–ray energy range. Using the new databases, we have extended PHOENIX to use many new spectral lines in the X–ray waveband down to 1 Å, improved data for electron collision rates, new data for proton collisionrates, andbetterdataforthermalbremsstrahlung. X–RAY OBSERVATIONS OF NOVA V4743 SGR The solid curve of Fig. 1 shows the observed X–ray spectrum of nova V4743 Sgr on March 19, 2003 with theLETGS onboard the CHANDRA satellite[2]. At wavelengths greater than ≈55Å, it is dominated by second and higher dispersion orders, and these wavelengths will not be considered in our analysis. The effective areas used to convert fromct s−1 to flux aredeterminedwiththeCIAO softwarepackage2, version3.0. An examination of the spectrum shows that it is not a black–body but resembles a stellar atmosphere with deep absorption features and, possibly, some weak emission lines. The strongest lines are from the two highest ionisation stages of C, N, and O. An extensiveanalysisoftheobservationhas been carried outby [2]. MODEL WITH SOLAR ABUNDANCES ThebestfitwithsolarabundancestothespectrumofnovaV4743SgrisshowninFig.1, leftpanel.ThemodelhasaneffectivetemperatureofT =5.8×105Kandabolometric eff luminosity of Lbol = 50,000L⊙. To get the correct slope for the pseudo–continuum, a value of n = 4.0×1021cm−2 for the hydrogen column density has to be used. The h quality of the fit is independent of the luminosityof the model. This was already found forearliersolarmodelsin otherwavelengthranges [4]. Close inspection of the measured spectrum reveals that some spectral lines are not reproduced well or are missing in the model spectrum. This is because we have used onlysolarabundances in thismodeland havenotincreased abundances of, forexample the CNO elements, as is generally observed in novae and predicted by theory [5]. Furthermore all absorption lines are too weak and there is too much emission around l ∼24Å. Increasing the abundances should increase the absorption and the fit should improvewithsolarabundances. The X–ray emission is dominated by thermal bremsstrahlung from the atmosphere surrounding the WD and the hard spectral range of l . 29Å is dominated by iron and nitrogen absorption. The atmosphere is in strong departure from LTE and is very extendedwiththehighestionizationstages ofelementsintheoutestlayers. 1 http://cxc.harvard.edu/atomdb/ 2 http://cxc.harvard.edu/ciao/ FIGURE1. ModelatmosphereofnovaV4743Sgrwithsolar(left)andnon–solarabundances(right). Thesolidcurveistheobservedspectrum. MODEL WITH NON–SOLAR ABUNDANCES A model with non–solar abundances (Fig. 1, right panel) produces a spectrum which fits the observationmuch betterthan with solar abundances. It was calculated with a 22 timessolarabundanceofnitrogenandoxygen.Accordinglythenitrogentooxygenratio isequaltothesolarvalue.Theabundanceofcarbonwith1.25timessolarisonlyslightly higherthanin solarmaterial. The strengths of some spectral lines now fit much better to the observation. For example, the fits of the N VII line at l ∼ 24.8Å and the O VII line at l ∼ 21.6Å. Aroundl ∼24Å thereisstilltoo muchemission. ACKNOWLEDGMENTS SomeofthecalculationspresentedherewereperformedattheHöchstleistungsRechen- zentrum Nord (HLRN) and at the National Energy Research Supercomputer Center (NERSC), supported by the U.S. DOE. We thank all these institutions for a generous allocation of computer time. Part of this work was supported by the DFG (Deutsche Forschungsgemeinschaft),projectnumberHA3457/2–1.S.Starrfield waspartiallysup- portedby grantsfromNASA–CHANDRA, NASA–Theory,and NSFto ASU. REFERENCES 1. Petz,A.,Hauschildt,P.H.,Ness,J.U.,&Starrfield,S.2004,AstroPh-0410370 2. Ness,J.U.,Starrfield,S.,Burwitz,V.,etal.2003,ApJ,594,L127 3. Young,P.R.,Zanna,G.D.,Landi,E.,etal.2003,ApJS,144,135 4. Hauschildt,P.H.&Starrfield,S.1995,ApJ,447,829 5. Starrfield,S.,Truran,J.W.,Wiescher,M.C.,&Sparks,W.M.1998,MNRAS,33,804