2014A&A...570A..25D


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.15CEST19:55:43

2014A&A...570A..25D - Astronomy and Astrophysics, volume 570A, 25-25 (2014/10-1)

Binary evolution using the theory of osculating orbits. I. Conservative Algol evolution.

DAVIS P.J., SIESS L. and DESCHAMPS R.

Abstract (from CDS):

Studies of conservative mass transfer in interacting binary systems widely assume that orbital angular momentum is conserved. However, this only holds under physically unrealistic assumptions. Our aim is to calculate the evolution of Algol binaries within the framework of the osculating orbital theory, which considers the perturbing forces acting on the orbit of each star arising from mass exchange via Roche lobe overflow. The scheme is compared to results calculated from a ``classical'' prescription. Using our stellar binary evolution code BINSTAR, we calculate the orbital evolution of Algol binaries undergoing case A and case B mass transfer, by applying the osculating scheme. The velocities of the ejected and accreted material are evaluated by solving the restricted three-body equations of motion, within the ballistic approximation. This allows us to determine the change of linear momentum of each star, and the gravitational force applied by the mass transfer stream. Torques applied on the stellar spins by tides and mass transfer are also considered. Using the osculating formalism gives shorter post-mass transfer orbital periods typically by a factor of 4 compared to the classical scheme, owing to the gravitational force applied onto the stars by the mass transfer stream. Additionally, during the rapid phase of mass exchange, the donor star is spun down on a timescale shorter than the tidal synchronization timescale, leading to sub-synchronous rotation. Consequently, between 15 and 20 per cent of the material leaving the inner-Lagrangian point is accreted back onto the donor (so-called ``self-accretion''), further enhancing orbital shrinkage. Self-accretion, and the sink of orbital angular momentum which mass transfer provides, may potentially lead to more contact binaries. Even though Algols are mainly considered, the osculating prescription is applicable to all types of interacting binaries, including those with eccentric orbits.

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Journal keyword(s): binaries: general - stars: evolution - stars: rotation - stars: mass-loss - celestial mechanics

Simbad objects: 15

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Number of rows : 15

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 V* TV Cas Al* 00 19 18.7424190416 +59 08 20.541942509 7.27 7.29 7.22     B9V 260 0
2 V* RX Cas bL* 03 07 45.7481570255 +67 34 38.614798549   10.14 8.64     K1III+A5eIII 173 0
3 HD 35921 bL* 05 29 42.65002 +35 22 30.0896 6.23 6.96 6.85     O9II 227 0
4 V* AR Mon RS* 07 20 48.4540808090 -05 15 35.799308532   9.84 8.79   7.608 G6IV 160 0
5 V* UX Mon Al* 07 59 16.3751282592 -07 30 17.889948033   8.74 8.42     A2/3+G/K 123 0
6 V* TX UMa Al* 10 45 20.5033114027 +45 33 58.703967287   6.99 6.98     B8V+G0III-IV 271 0
7 V* TU Mus bL* 11 31 10.9242217305 -65 44 32.098796901 7.58 9.52 9.34 9.25   O8V(n)z+B0V(n) 145 0
8 V* SV Cen WU* 11 47 57.2195336815 -60 33 57.757259516 7.98 9.71 9.70 9.46 8.810 B1/3 132 0
9 HD 139319 ** 15 33 51.05705 +63 54 25.6950           ~ 233 0
10 HD 139319A SB* 15 33 51.0598928122 +63 54 25.706692279   7.75 7.46     A5m 237 0
11 * bet Lyr bL* 18 50 04.7952472 +33 21 45.609978 2.85 3.42 3.42 3.31 3.29 B8.5Ib-II 882 0
12 TYC 3547-2135-1 bL* 19 21 11.6185430446 +47 58 42.954059789   9.79 9.53   9.330 A5IV 42 0
13 V* V382 Cyg bL* 20 18 47.2203014045 +36 20 26.091543194 9.35 9.19 8.65     O6IVn+O5Vn 171 0
14 HD 199005 ** 20 58 40.09745 -70 25 19.7765           F6V 56 0
15 HD 199005A Al* 20 58 40.1052033066 -70 25 19.714290422   8.28 7.85 8.67   ~ 55 0

    Equat.    Gal    SGal    Ecl

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2019.10.15-19:55:43

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