1. X-ray Grating Spectroscopy of Cataclysmic Variables
Christopher Mauche
Lawrence Livermore National Laboratory
X-ray Grating Spectroscopy  Cambridge, MA  2007 July 11–13

2. Accretion geometry and X-ray emission
regions of magnetic & nonmagnetic CVs
X-ray
EUV
white dwarf
Magnetic CV (polar)
disk
white dwarf
EUV
X-ray
Nonmagnetic CV (dwarf nova, novalike variable)

3. Accretion geometry and X-ray emission
regions of intermediate polars (EX Hya)
X-ray
EUV
white dwarf
spin min
spin max
Hellier et al. (1987); Rosen, Mason, & Córdova (1988)

4. EUVE SW and Chandra LETG spectra of
nonmagnetic CVs

5. EUVE SW and Chandra LETG spectra of
nonmagnetic CVs

6. Chandra LETG spectra of nonmagnetic CVs

7. The EUV flux of SS Cyg oscillates but the X-ray flux does not
Does not oscillate
Oscillates
DNO
QPO
 CVs
NS 
BH  
Mauche (2002, ApJ, 580, 423)
[Warner et al. 2003, MNRAS, 344, 1193]

8. EUV flux is not eclipsed by the white dwarf
EUVE DS light curves of OY Car
EUV flux is not eclipsed by the white dwarf
Mauche & Raymond (2000, ApJ, 541, 924)

9. Model of the EUVE SW spectrum of OY Car
Mauche & Raymond (2000, ApJ, 541, 924)

10. Model of the Chandra LETG spectrum of SS Cyg
Mauche (2004, ApJ, 610, 422)

11. Chandra LETG spectrum of WZ Sge
O VI 2s-2p
150 (Chandra)
1032,1038 (FUSE)
Wheatley & Mauche (2007, in preparation)

12. XMM EPIC light curves and spectra show
two sources of X-ray emission in UX UMa
Hard X-ray flux is eclipsed
Soft X-ray flux is not
Multi-T
NH
kT~5 keV
NH
Pratt et al. (2004, MNRAS, 348, L49)

13. Chandra LETG spectrum of AM Her
Ne IX
O VIII
O VII
Burwitz et al. (2002, ASPC, 261, 137); Burwitz (2006, in High
Resolution X-ray Spectroscopy: Towards XEUS and Con-X);

14. Chandra LETG light curves and spectrum of AM Her
Out of eclipse
Scaled eclipse

15. Two types of X-ray spectra in CVs
Cooling Flow
Photoionized
Mukai et al. (2003, ApJ, 586, 77)

16. Chandra HETG spectra of nonmagnetic
CVs

17. Chandra HETG spectra of SS Cyg in quiescence and outburst
X-ray flux decreases in outburst, lines broaden.
Mauche et al. (2005, in Astrophysics of CVs & Related Objects)

18. Chandra HETG spectra of U Gem in quiescence and outburst
X-ray flux increases in outburst, lines broaden.
Szkody et al. (2002, ApJ, 574, 942)
Mauche et al. (2005, in Astrophysics of CVs & Related Objects)
Güver et al. (2006, MNRAS, 372, 450)

19. Fe K emission lines in Chandra HETG spectra of six nonmagnetic CVs
Rana et al. (2006, ApJ, 642, 1042)

20. Fe K emission lines in Chandra HETG
spectra of U Gem & SS Cyg in outburst
 The Fe XXV emission lines in U Gem in outburst is broadened by ~ 2500 km s-1.
 The fluorescent Fe line in SS Cyg in outburst is redshifted by ~ 2300 km s-1 (z=GM/Rc2 ~ 100 km s-1)
Rana et al. (2006, ApJ, 642, 1042)

21. Chandra HETG spectrum of V603 Aql
Mukai & Orio (2005, ApJ, 622, 602)

22. Chandra HETG spectra of IPs
 Fluorescent Fe line

23. Chandra HETG spectrum of GK Per
Al XI ?
Ne IX RRC ? 

24. Fe K emission lines in Chandra HETG spectra of five magnetic CVs
Contrary to previous claims (Hellier, Mukai & Osborne
1998), these lines are not signif. Compton broadened.
Hellier & Mukai (2004, MNRAS, 352, 1037)

25. 500 ks observation, N. Brickhouse, PI
Chandra HETG spectrum of EX Hya (an IP
with Pbinary = 98 min, Pspin = 67 min, i  77o)
500 ks observation, N. Brickhouse, PI

26. Comparison of HR 1099 and EX Hya22 | 21 17
| |
Ne IX
| | | 20
EX Hya is missing lines of: Fe XVII 17.10,
Fe XX 12.80, Fe XXI 12.26, and has an
inverted Fe XXII 11.92/11.77 ratio.
Mauche, Liedahl, & Fournier (2005, in X-ray Diagnostics of
Astrophysical Plasmas: Theory, Experiment, & Observation)

27. H- and He-like lines of EX Hya
All the He-like f lines are missing in EX Hya.
Mauche (2002, in Physics of CVs and Related Objects)

28. He-like R = z/(x+y) = f/i line ratios
Tbb = 0 K
Tbb = 30 kK
Absence of He-like f lines in EX Hya
is plausibly due to photoexcitation.
Mauche (2002, in Physics of CVs and Related Objects)

29. Theoretical Fe L-shell spectra
…were calculated with the Livermore X-ray Spectral Synthesizer (LXSS), a suite of IDL codes that calculates spectral models as a function of temperature and electron density using primarily HULLAC atomic data.
The following spectra are based on models with:
Ion levels radrate colrate
Fe XXIV 76 4,100 1,704
Fe XXIII 116 8,798 6,478
Fe XXII ,300 24,084
Fe XXI , ,953
Fe XX , ,350
Fe XIX , ,496
Fe XVIII ,229 93,583
Fe XVII ,882 33,887
Mauche, Liedahl, & Fournier (2005, in X-ray Diagnostics of
Astrophysical Plasmas: Theory, Experiment, & Observation)

30. Fe XVII  Red: 1010 cm3 Blue: 1018 cm3
Mauche, Liedahl, & Fournier (2005, in X-ray Diagnostics of
Astrophysical Plasmas: Theory, Experiment, & Observation)

31. Fe XVIII Red: 1010 cm3 Blue: 1018 cm3
Mauche, Liedahl, & Fournier (2005, in X-ray Diagnostics of
Astrophysical Plasmas: Theory, Experiment, & Observation)

32. Fe XIX
Red: 1010 cm3
Blue: 1018 cm3
Mauche, Liedahl, & Fournier (2005, in X-ray Diagnostics of
Astrophysical Plasmas: Theory, Experiment, & Observation)

33. Fe XX 
Red: 1010 cm3
Blue: 1018 cm3
Mauche, Liedahl, & Fournier (2005, in X-ray Diagnostics of
Astrophysical Plasmas: Theory, Experiment, & Observation)

34. Fe XXI 
Red: 1010 cm3
Blue: 1018 cm3
Mauche, Liedahl, & Fournier (2005, in X-ray Diagnostics of
Astrophysical Plasmas: Theory, Experiment, & Observation)

35. Fe XXII  Red: 1010 cm3 Blue: 1018 cm3
Mauche, Liedahl, & Fournier (2005, in X-ray Diagnostics of
Astrophysical Plasmas: Theory, Experiment, & Observation)

36. Fe XXIII Red: 1010 cm3 Blue: 1018 cm3
Mauche, Liedahl, & Fournier (2005, in X-ray Diagnostics of
Astrophysical Plasmas: Theory, Experiment, & Observation)

37. Fe XXIV
Red: 1010 cm3
Blue: 1018 cm3
Mauche, Liedahl, & Fournier (2005, in X-ray Diagnostics of
Astrophysical Plasmas: Theory, Experiment, & Observation)

38. Grotrian diagrams for Fe XVII and Fe XXII
Mauche, Liedahl, & Fournier (2005, in X-ray Diagnostics of
Astrophysical Plasmas: Theory, Experiment, & Observation)

39. Density constraints from Fe XVII 17. 10/17. 05 and Fe XXII 11
Fe XVI: ne > 2x1014 cm-3
Mauche, Liedahl, & Fournier (2001, ApJ, 560, 992)
Mauche, Liedahl, & Fournier (2003, ApJ, 588, L101)
Fe XXII: ne ~ 1x1014 cm-3

40. Radial velocity variations of the X-ray emission lines of EX Hya
 = 1.3 +/- 2.3 km s-1
K = /- 3.7 km s-1
Mwd = / M
bin
Dynamically-derived white dwarf mass agrees
with the value obtained from the Fe XXV/XXVI
line ratio in the ASCA SIS spectrum of EX Hya
(Fujimoto & Ishida 1997).
Hoogerwerf, Brickhouse, & Mauche (2004, ApJ, 610, 411)

41. Chandra HETG spectrum of AE Aqr (an IP
with Pbinary = 9.88 hr, Pspin = s, i  60o)
Different physical models for AE Aqr:
Patterson (1979)
Wynn, King, & Horne (1997)
Magnetic propeller model
Oblique rotator model

42. XMM EPIC & RGS spectra of AE Aqr
4T VMEKAL:
kT = 0.14, 0.59, 1.21, & 4.6 keV
(cool for an IP)
Itoh et al. (2006, ApJ, 639, 397)

43. ne ~ 1011 cm-3 : low for a magnetic CV
He-like N, O, & Ne density diagnostics from the XMM RGS spectrum of AE Aqr
ne ~ 1011 cm-3 : low for a magnetic CV
Itoh et al. (2006, ApJ, 639, 397)

44. X-ray, UV, optical, & radio light curves of AE Aqr
Chandra HETG
GALEX NUV B
VLA 3.6 cm V
Optical: Ioannou (Skinakas), Welsh (Laguna), CBA, & AAVSO
Radio: Abada-Simon & Desmurs
Strong correlation of the flares in the X-ray, UV,
and optical, but not in the radio.
Mauche et al. (2007, in preparation)

45. Spin-down evolution of the white dwarf in AE Aqr
optical
X-ray
“Discovery of a brake in AE Aqr”
de Jager et al. (1994)
P = 5.64x10-14 d d-1
Spin-down power Lsd = -I
= 6x1033 I50 erg s-1 >> Lx
P = 2.0(1.0)x10-15 d d-1 or
P = 3.46(56)x10-19 d-1
“AE Aqr brakes harder”
Mauche (2006)*  
The P term is inconsistent in sign and magnitude
with magnetic dipole radiation losses (cf. Ikhsanov
1998, who ascribes P in AE Aqr to magnetic dipole radiation losses of a white dwarf with B ~ 50 MG).  
*Mauche (2006, MNRAS, 369, 1983)

46. Pulse-timing delays of AE Aqr
Optical:
a sini = / s
de Jager et al. (1994)
HST FOS UV:
a sini = / s
Eracleous et al. (1994)
Chandra HETG X-ray:
a sini = / s
Mauche (2006)*
Pulsating optical, UV, & X-ray source follows the motion of the white dwarf.
*Mauche (2006, MNRAS, 369, 1983)

47. AE Aqr spin-phase light curves and radial velocity variation
 = 33 +/- 24 km s-1
K = 154 +/- 38 km s-1
0 = /
[z = GM/Rc2 ~ 50 km s-1]
X-ray emission line radial velocities consistent with emission from two poles.
Mauche (2007, in preparation)

48. Acknowledgements
Support for this work was provided by NASA through Chandra Award Number GO5-6021X issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS This work was performed under the auspices of the US Department of Energy by the University of California Lawrence Livermore National Laboratory under contract W-7405-Eng-48.