Kitaguchi, Takao3; An, Hongjun3; Beloborodov, Andrei M.3; Gotthelf, Eric V.3; Hayashi, Takayuki3; Kaspi, Victoria M.3; Rana, Vikram R.3; Boggs, Steven E.3; Christensen, Finn Erland1; Craig, William W.3; Hailey, Charles J.3; Harrison, Fiona A.3; Stern, Daniel3; Zhang, Will W.3
1 National Space Institute, Technical University of Denmark2 Astrophysics, National Space Institute, Technical University of Denmark3 unknown
AE Aquarii is a cataclysmic variable with the fastest known rotating magnetized white dwarf (P-spin = 33.08 s). Compared to many intermediate polars, AE Aquarii shows a soft X-ray spectrum with a very low luminosity (L-X similar to 10(31) erg s(-1)). We have analyzed overlapping observations of this system with the NuSTAR and the Swift X-ray observatories in 2012 September. We find the 0.5-30 keV spectra to be well fitted by either an optically thin thermal plasma model with three temperatures of 0.75(-0.45)(+0.18), 2.29(-0.82)(+0.96), and 9.33(-2.18)(+6.07) keV, or an optically thin thermal plasma model with two temperatures of 1.00(-0.23)(+0.34) and 4.64(-0.84)(+1.58) keV plus a power-law component with photon index of 2.50(-0.23)(+0.17). The pulse profile in the 3-20 keV band is broad and approximately sinusoidal, with a pulsed fraction of 16.6% +/- 2.3%. We do not find any evidence for a previously reported sharp feature in the pulse profile.
Astrophysical Journal, 2014, Vol 782, Issue 1
ASTRONOMY; X-RAY PULSATIONS; CATACLYSMIC VARIABLES; INTERMEDIATE POLARS; LINE DIAGNOSTICS; ACCRETION FLOWS; HOT PLASMA; XMM-NEWTON; EMISSION; TELESCOPE; SPECTRA; accretion, accretion disks; novae, cataclysmic variables; stars: individual (AE Aquarii); white dwarfs; X-rays: stars; accretion accretion disks; Novae cataclysmic variables; Stars: individual (AE Aquarii); White dwarfs; X-rays:stars