2011A&A...532A.129T


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.10CEST02:37:07

2011A&A...532A.129T - Astronomy and Astrophysics, volume 532A, 129-129 (2011/8-1)

Accretion in the detached post-common-envelope binary LTT 560.

TAPPERT C., GAENSICKE B.T., SCHMIDTOBREICK L. and RIBEIRO T.

Abstract (from CDS):

In a previous study, we found that the detached post-common-envelope binary LTT 560 displays an Hα emission line consisting of two anti-phased components. While one of them was clearly caused by stellar activity from the secondary late-type main-sequence star, our analysis indicated that the white dwarf primary star is potentially the origin of the second component. However, the low resolution of the data means that our interpretation remains ambiguous. We here use time-series UVES data to compare the radial velocities of the Hα emission components to those of metal absorption lines from the primary and secondary stars. We find that the weaker component most certainly originates in the white dwarf and is probably caused by accretion. An abundance analysis of the white dwarf spectrum yields accretion rates that are consistent with mass loss from the secondary due to a stellar wind. The second and stronger Hα component is attributed to stellar activity on the secondary star. An active secondary is likely to be present because of the occurrence of a flare in our time-resolved spectroscopy. Furthermore, Roche tomography indicates that a significant area of the secondary star on its leading side and close to the first Lagrange point is covered by star spots. Finally, we derive the parameters for the system and place it in an evolutionary context. We find that the white dwarf is a very slow rotator, suggesting that it has had an angular-momentum evolution similar to that of field white dwarfs. We predict that LTT 560 will begin mass transfer via Roche-lobe overflow in ∼3.5Gyr, and conclude that the system is representative of the progenitors of the current population of cataclysmic variables. It will most likely evolve to become an SU UMa type dwarf nova.

Abstract Copyright:

Journal keyword(s): binaries: close - stars: late-type - white dwarfs - stars: individual: LTT 560 - novae, cataclysmic variables

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 G 269-70 CV* 00 59 28.8887547784 -26 31 05.657727154   16.22 15.94     M5.5 37 0
2 V* XX Tri RS* 02 03 47.1138016857 +35 35 28.669244792   9.52 8.42     K0III 117 0
3 V* V471 Tau Al* 03 50 24.9664598642 +17 14 47.433240686   10.258 9.373   8.393 K2V+DA 615 0
4 V* RR Cae WD* 04 21 05.5631969817 -48 39 07.062891386 14.50 14.92 14.40     DA7.8 134 1
5 V* SU UMa DN* 08 12 28.2694633475 +62 36 22.428029272           B2 469 0
6 CD-30 17706 WD* 20 10 56.8485174654 -30 13 06.629141494 11.654 12.286 12.242 12.311 12.381 DA3.1 219 0

    Equat.    Gal    SGal    Ecl

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2020.07.10-02:37:07

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