1. Institute for Astronomy and Astrophysics, University of Tübingen 13 July 2007X-ray Grating Spectroscopy Cambridge, USA 1 X-ray Photospheres Klaus Werner Institute for Astronomy and Astrophysics, University of Tübingen, Germany

2. Institute for Astronomy and Astrophysics, University of Tübingen 13 July 2007X-ray Grating Spectroscopy Cambridge, USA 2 Outline Introduction: Thermal soft X-ray emission from stellar photospheres Chandra spectroscopy of the hot DA white dwarf LB1919: Implications for vertical chemical stratification in WDs Chandra spectroscopy of the PG1159 star PG1520+525: Constraining the GW Vir instability strip in the HRD Chandra spectroscopy of the naked C/O stellar core H1504+65: The hottest known and chemically most extreme white dwarf

3. Introduction Only evolved compact stars are hot enough to be able to emit thermal (soft) X-radiation from their photosphere: Neutron stars (not covered in this talk) (Pre-) white dwarfs (WDs), (some are central stars of PNe) WDs come in two flavors: Hydrogen-rich (DA WDs) Helium and/or C-O-rich (non-DAs), relevant here: PG1159 stars, the hottest non-DA WDs

4. Introduction Hydrogen-rich WDs: Photospheres of hot DAs are almost completely ionized, hence, very low opacity. Observed X-rays stem from very deep, hot layers. Soft X-rays are detected from objects with T eff >30,000 K Famous example: Sirius B He-C-O-rich (non-DA) WDs: Opacities of He and metals prevent leakage of X-rays from deep hot layers, except for hottest objects, where these species are highly ionised and more transparent: Soft X-rays are detected from objects with T eff >140,000 K Famous example: H1504+65

5. Outline Introduction: Thermal soft X-ray emission from stellar photospheres Chandra spectroscopy of the hot DA white dwarf LB1919: Implications for vertical chemical stratification in WDs Chandra spectroscopy of the PG1159 star PG1520+525: Constraining the GW Vir instability strip in the HRD Chandra spectroscopy of the naked C/O stellar core H1504+65: The hottest known and chemically most extreme white dwarf

6. Metals as sensitive regulators of X-rays from DA white dwarfs Hydrogen in hot DAs almost completely ionized, EUV/soft X-ray opacity strongly reduced → DAs with T eff >30,000 K can emit thermal soft X-rays from deep hot layers However, ROSAT All-Sky Survey revealed that X-ray emission is the exception rather than the rule → additional absorbers present ROSAT and EUVE revealed that metals are the origin, EUV spectra are strongly determined by Fe and Ni through large number of absorption lines Radiative levitation keeps traces of metals in the atmosphere (e.g. Chayer et al. 1995): Generally, metal abundances increase with increasing T eff. Consequently, only very few DAs with T eff >60,000 K were detected in EUVE and ROSAT All-Sky Surveys.

7. Breakthrough in understanding DA atmospheres: development of self-consistent models for equilibrium of gravitational settling / radiative levitation, yield vertical abundance stratification Generally, good agreement between observed and computed EUV flux distributions (e.g. Schuh et al. 2002) However, several exceptions are known. Some DAs show much larger metal abundances than expected from theory, reason: ISM accretion or wind-accretion from unseen companion More difficult to explain: objects with metallicity smaller than expected

8. The problem of metal-poor DA white dwarfs Prominent example: HZ43 (T eff = 49,000 K), virtually metal free, shows no EUV or X-ray absorption features Even more surprising: low metallicity of two DAs with even higher T eff. Two of hottest known DAs have extraordinarily low metal abundances: LB1919 (69,000 K) & MCT0027-6341 (60,000 K) These stars could hold the key to understanding metal-poor DAs as a class We concentrate on LB1919, it is brighter in EUV/X-rays LB1919: hottest of the 90 DAs detected in EUVE all-sky survey (Vennes et al. 1997). Hottest of the 20 DAs whose EUVE spectra were analyzed in detail by Wolff et al. (1998) Chemical composition unknown: EUVE resolution insufficient to resolve individual lines; metallicity of fainter DAs usually determined relative to G191-B2B (56,000 K) that is well studied by UV spectroscopy.

9. Our stratified models successfully describe the EUV spectrum of G191-B2B. EUVE spectra of other DAs could also be fitted by simply scaling G191´s relative metal abundance pattern. But: the EUV spectrum of LB1919 cannot be described by chemically homogeneous models scaled to G191 relative abundances. Also, radiatively stratified models fail spectacularly. The problem of metal-poor DA white dwarfs

10. Four processes can disturb equilibrium between gravitation and levitation; potentially responsible for metal-poor hot DAs: Mass-loss tends to homogenize chemical stratification. However, M-dot drops below critical limit (10 -16 M  /yr) for T eff <70,000 K (Unglaub & Bues 1998). So, LB1919 should not be affected. Wind-accretion calculations (MacDonald 1992) show that ISM accretion is prevented for LB1919 since its L>1L . Instead, mass- loss rate of 10 -18 M  /yr will be sustained Convection not expected in LB1919 Rotation could lead to meridional mixing, however, WDs are generally slow rotators. In particular, LB1919 shows sharp Lyman line cores (FUSE), ruling out high rotation rate. Currently there is no explanation for the low metallicity in LB1919 and similar DAs

11. Chandra observation of LB1919 Aim: Empirical determination of abundance stratification using individual lines of different ionization stages of Fe, Ni... IF metals are stratified, then they are in diffusion/levitation equilibrium. The low metallicity might originate in earlier evolutionary phases (selective radiation driven wind?) IF metals are homogeneous, then one of the above mechanisms is at work, contrary to our understanding

12. Individual lines can in principle be identified in Chandra spectra, as was shown for the hot DA GD 246 (Vennes et al. 2002). GD 246 - Chandra

13. Simulated Chandra observations of LB1919 LETG+HRC-S, 120 ksec Parameters of LB1919: T eff =70,000 K logg=8.2 Fe/H=7.5∙10 -7 Ni/H=5∙10 -8 (EUVE analysis of Wolff et al. 1998 with homogeneous models) Two models shown: a) nickel enhanced by 1 dex (black line) b) iron and nickel enhanced by 1 dex (red line) Strong sensitivity of the spectrum against abundance variations

14. Chandra observation of LB1919 Low Energy Transmission Grating (LETG+HRC-S) Integration time 111 ksec, Feb. 02, 2006

15. Low Energy Transmission Grating (LETG+HRC-S) Integration time 111 ksec, Feb. 02, 2006 Line features in model too strong, analysis is on-going, no results yet Chandra observation of LB1919

16. Outline Introduction: Thermal soft X-ray emission from stellar photospheres Chandra spectroscopy of the hot DA white dwarf LB1919: Implications for vertical chemical stratification in WDs Chandra spectroscopy of the PG1159 star PG1520+525: Constraining the GW Vir instability strip in the HRD Chandra spectroscopy of the naked C/O stellar core H1504+65: The hottest known and chemically most extreme white dwarf

17. The PG1159 spectroscopic class, a group of 40 stars Very hot hydrogen-deficient (pre-) WDs T eff = 75,000 – 200,000 K log g= 5.5 – 8 M/M  = 0.51 – 0.89 (mean: 0.62) log L/L  = 1.1 – 4.2 Atmospheres dominated by C, He, O, and Ne, e.g. prototype PG1159-035: He=33%, C=48%, O=17%, Ne=2% (mass fractions) = chemistry of material between H and He burning shells in AGB-stars (intershell abundances)

18. Evolutionary tracks for a 2 M  star. Born-again track offset for clarity. (Werner & Herwig 2006) late He-shell flash causes return to AGB

19. Loss of H-rich envelope consequence of (very) late thermal pulse during post-AGB phase (LTP) or WD cooling phase (VLTP) (like Sakurai’s object and FG Sge) Hydrogen envelope (thickness 10 -4 M  ) is ingested and burned (VLTP) or diluted (LTP) in He-rich intershell (thickness 10 -2 M  ) In any case, composition of He/C/O-rich intershell region dominates complete envelope on top of stellar C/O core

20. Late He-shell flash +CO core material (dredged up) 10 -2 M  10 -4 M 

21. Pulsating (filled circles) and non-pulsating PG1159 stars Blue (Gautschy et al. 2005) and red (Quirion et al. 2004) edges of GW Vir instability strip 0.6 M  track (Wood & Faulkner 1986) PG1520+525 PG1159-035

22. The pulsator/non-pulsator pair PG 1159-035 and PG 1520+525 Very similar atmospheric parameters PG1159-035PG1520+525 T eff 140,000150,000 log g7.07.5 He0.330.43 C0.480.38 O0.17 Ne0.02 Mass/M  0.600.67

23. Do both stars confine the blue edge of the instability strip? To what accuracy is their T eff known? PG1159-035: 140,000 +/- 5,000 K from HST/STIS high-resolution UV spectrum, Jahn et al. (2007) PG1520+525: 150,000 +/- 15,000 K from HST/GHRS medium-resolution UV spectrum, Dreizler & Heber (1998) Need a more precise T eff estimate for PG1520+525 Try soft X-ray region; PG1520+525 is the soft X-ray brightest PG1159 star after H1504+65. First attempt with EUVE suggested T eff around 150,000 K, however, poor-S/N spectrum The pulsator/non-pulsator pair PG 1159-035 and PG 1520+525

24. Werner et al. (1996)

25. Soft X-ray spectral modeling of PG 1520+525 Grid of non-LTE models (hydrostatic, radiative equilibrium) Ions included: He I-III, C III-V, O IV-VII, Ne IV-IX, Mg IV-IX Particular model shown here tailored to PG1520+525 For comparison with Chandra observation: model flux used to simulate Chandra count rate spectrum including expected S/N

26. Chandra observation of PG 1520+525 Low Energy Transmission Grating (LETG+HRC-S) Integration time 142 ksec, April 04-06, 2006

27. Chandra observation of PG 1520+525 Low Energy Transmission Grating (LETG+HRC-S) Integration time 142 ksec, April 04-06, 2006

28. Detail of PG 1520+525 Chandra spectrum, 100-123 Å model observation

29. Detail of PG 1520+525 Chandra spectrum, 100-123 Å Identification of OVI and NeVI / VII lines OVI NeVII OVI NeVI NeVII NeVI model observation

30. FUV studies of PG1520+525 Element abundances affect soft X-ray flux, but due to difficult line identification there, constraints must be provided from other observations Crucial: FUSE spectroscopy. All identified species in PG1520+525 display lines in this wavelength region. Besides presence of He, C, O: First identification of silicon, sulfur, phosphorus abundance determinations by Reiff et al. (2007) First identification of neon and fluorine strongly over-solar abundances (Werner et al. 2004, 2005)

31. First discovery of fluorine in hot post-AGB stars: F VI 1139.50 Å F abundance in PG1520+525: 200 times solar PG1159-035: 10 times solar

32. 140,000 K model too cool, good fit with 150,000 K model.

33. Pulsating (filled circles) and non-pulsating PG1159 stars PG1159-035 and PG1520+525 indeed confine the blue edge of the GW Vir instability strip 0.6 M  track (Wood & Faulkner 1986) PG1520+525 PG1159-035

34. Outline Introduction: Thermal soft X-ray emission from stellar photospheres Chandra spectroscopy of the hot DA white dwarf LB1919: Implications for vertical chemical stratification in WDs Chandra spectroscopy of the PG1159 star PG1520+525: Constraining the GW Vir instability strip in the HRD Chandra spectroscopy of the naked C/O stellar core H1504+65: The hottest known and chemically most extreme white dwarf

35. Properties of H1504+65 1983 – H1504 is the 7th brightest X-ray source in the 0.25 keV band (HEAO1 survey, Nugent et al.) 1986 – Optical identification: Extremely hot white dwarf, lacking H and He lines (Nousek et al.) 1991 – NLTE analysis of optical spectra (Werner): It is the hottest WD known (T eff close to 200 000 K) H1504 is devoid of hydrogen and helium Dominant photospheric species: C and O (50:50) 1999 – Analysis of EUVE & Keck data (Werner & Wolff) High neon abundance: 2-5% (>20 times solar) H1504 is an extreme member of the PG1159 spectroscopic class

36. Chandra LETG+HRC-S observation of H1504+65: Sept. 27, 2000, integration time 7 hours Richest absorption line spectrum ever recorded from a stellar photosphere (Werner et al. 2004, A&A 421, 1169) Examples for spectral fitting:

37. Model fit to H1504+65 Chandra spectrum 80-110 Å Wavelength / Å Relative flux

38. Model fit to H1504+65 Chandra spectrum 80-110 Å Wavelength / Å Relative flux

39. Model fit to H1504+65 Chandra spectrum 80-110 Å Wavelength / Å Relative flux

40. Model fit to H1504+65 Chandra spectrum 110-140 Å Wavelength / Å Relative flux

41. Model fit to H1504+65 Chandra spectrum 110-140 Å Wavelength / Å Relative flux

42. Model fit to H1504+65 Chandra spectrum 110-140 Å Wavelength / Å Relative flux

43. Strong Fe-group line blanketing

46. Origin of unique C/O/Ne surface composition of H1504 remains unknown. Obviously, H1504 is a bare C/O core of a former AGB giant. Detection of Mg  2% in Chandra spectrum even suggests: H1504 could be a bare O/Ne/Mg white dwarf, i.e. first observational proof for existence of such objects Approved HST UV-spectroscopy (2005): Search for Na, but: failure of STIS just before observations should be done

47. Summary Hottest WDs have detectable photospheric soft X-ray emission X-ray grating spectroscopy important (and often essential) to derive stellar parameters and details of photospheric processes Results are relevant for our understanding of late phases of stellar evolution In detail: Chandra spectroscopy of a hot DA white dwarf and of two PG1159 stars Analysis of LB1919 will provide clues to answer the question why some hot DAs show a lower metallicity than expected from radiative levitation theory PG1520+525 confines the blue edge of the GW Vir instability strip (T eff =140,000—150,000 at logg=7) H1504+65 could turn out to be the first definitive proof for the existence of (single) O/Ne/Mg white dwarfs