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

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)

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)

EUVE SW and Chandra LETG spectra of nonmagnetic CVs

EUVE SW and Chandra LETG spectra of nonmagnetic CVs

Chandra LETG spectra of nonmagnetic CVs

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]

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)

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

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

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

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)

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);

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

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

Chandra HETG spectra of nonmagnetic CVs

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)

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)

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

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)

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

Chandra HETG spectra of IPs  Fluorescent Fe line

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

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)

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

Comparison of HR 1099 and EX Hya 22 | 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)

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)

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)

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 228 37,300 24,084 Fe XXI 591 227,743 153,953 Fe XX 609 257,765 165,350 Fe XIX 605 240,948 164,496 Fe XVIII 456 141,229 93,583 Fe XVII 281 49,882 33,887 Mauche, Liedahl, & Fournier (2005, in X-ray Diagnostics of Astrophysical Plasmas: Theory, Experiment, & Observation)

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

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

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

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

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

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

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

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

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

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

Radial velocity variations of the X-ray emission lines of EX Hya  = 1.3 +/- 2.3 km s-1 K = 58.2 +/- 3.7 km s-1 Mwd = 0.49 +/- 0.13 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)

Chandra HETG spectrum of AE Aqr (an IP with Pbinary = 9.88 hr, Pspin = 33.08 s, i  60o) Different physical models for AE Aqr: Patterson (1979) Wynn, King, & Horne (1997) Magnetic propeller model Oblique rotator model

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)

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)

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)

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)

Pulse-timing delays of AE Aqr Optical: a sini = 2.04 +/- 0.13 s de Jager et al. (1994) HST FOS UV: a sini = 1.93 +/- 0.03 s Eracleous et al. (1994) Chandra HETG X-ray: a sini = 2.17 +/- 0.48 s Mauche (2006)* Pulsating optical, UV, & X-ray source follows the motion of the white dwarf. *Mauche (2006, MNRAS, 369, 1983)

AE Aqr spin-phase light curves and radial velocity variation  = 33 +/- 24 km s-1 K = 154 +/- 38 km s-1 0 = 0.012 +/- 0.020 [z = GM/Rc2 ~ 50 km s-1] X-ray emission line radial velocities consistent with emission from two poles. Mauche (2007, in preparation)

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 NAS8-39073. 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.