2008A&A...480..199B


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.09CET23:04:53

2008A&A...480..199B - Astronomy and Astrophysics, volume 480, 199-212 (2008/3-2)

High-resolution spectroscopy of the intermediate polar EX Hydrae. I. Kinematic study and Roche tomography.

BEUERMANN K. and REINSCH K.

Abstract (from CDS):

object{EX Hya} is one of the few double-lined eclipsing cataclysmic variables that allow an accurate measurement of the binary masses. We analyze orbital phase-resolved UVES/VLT high resolution (λ/Δλ≃27000) spectroscopic observations of EX Hya with the aims of deriving the binary masses and obtaining a tomographic image of the illuminated secondary star. We present a novel method for determining the binary parameters by directly fitting an emission model of the illuminated secondary star to the phase-resolved line profiles of NaIλ8183/8195 in absorption and emission and CaIIλ8498 in emission. The fit to the NaI and CaII line profiles, combined with the published K1, yields a white-dwarf mass M1=0.790±0.026M, a secondary mass M2=0.108±0.008M, and a velocity amplitude of the secondary star K2=432.4±4.8km/s. The secondary is of spectral type dM5.5±0.5 and has an absolute K-band magnitude of MK=8.8. Its Roche radius places it on or very close to the main sequence of low-mass stars. It differs from a main sequence star by its illuminated hemisphere that faces the white dwarf. The secondary star contributes only 5% to the observed spin-phase averaged flux at 7500Å, 7.5% at 8200Å, and 37% in the K-band. We present images of the secondary star in the light of the NaI doublet and the CaII emission line derived with a simplified version of Roche tomography. Line emission is restricted to the illuminated part of the star, but its distribution differs from that of the incident energy flux. We have discovered narrow spectral lines from the secondary star in EX Hya that delineate its orbital motion and allow us to derive accurate masses of both components. The primary mass significantly exceeds recently published values. The secondary is a low-mass main sequence star that displays a rich emission line spectrum on its illuminated side, but lacks chromospheric emission on its dark side.

Abstract Copyright:

Journal keyword(s): methods: data analysis - stars: novae, cataclysmic variables - stars: fundamental parameters - stars: individual: EX Hya - stars: late-type - stars: white dwarfs

Errata: + corrigendum vol. 555, p. C1 (2013)

Simbad objects: 6

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Number of rows : 6

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 V* Z Cha DN* 08 07 27.7421647579 -76 32 00.679589237   12.00       M5.5 585 1
2 L 674-15 PM* 08 12 40.8887006440 -21 33 06.982376130   13.7 12.131 11.753 9.24 M3.5V 74 0
3 Wolf 359 Fl* 10 56 28.826208 +07 00 52.34400 16.706 15.541 13.507 11.684 9.507 M6Ve 623 0
4 Wolf 424 ** 12 33 17.361480 +09 01 15.79224 15.398 14.313 12.467 10.937 8.988 M5.5V 292 0
5 V* EX Hya DN* 12 52 24.2220533405 -29 14 56.001981146   13.51 13.49 13.55   M5-6V 645 0
6 V* V645 Cen Fl* 14 29 42.9451234609 -62 40 46.170818907 14.21 12.95 11.13 9.45 7.41 M5.5Ve 899 0

    Equat.    Gal    SGal    Ecl

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2019.12.09-23:04:53

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