2015A&A...573A.107H


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST08:43:03

2015A&A...573A.107H - Astronomy and Astrophysics, volume 573A, 107-107 (2015/1-1)

Properties and nature of Be stars. 30. Reliable physical properties of a semi-detached B9.5e+G8III binary BR CMi = HD 61273 compared to those of other well studied semi-detached emission-line binaries.

HARMANEC P., KOUBSKY P., NEMRAVOVA J.A., ROYER F., BRIOT D., NORTH P., LAMPENS P., FREMAT Y., YANG S., BOZIC H., KOTKOVA L., SKODA P., SLECHTA M., KORCAKOVA D., WOLF M. and ZASCHE P.

Abstract (from CDS):

Reliable determination of the basic physical properties of hot emission-line binaries with Roche-lobe filling secondaries is important for developing the theory of mass exchange in binaries. It is a very hard task, however, which is complicated by the presence of circumstellar matter in these systems. So far, only a small number of systems with accurate values of component masses, radii, and other properties are known. Here, we report the first detailed study of a new representative of this class of binaries, BR CMi, based on the analysis of radial velocities and multichannel photometry from several observatories, and compare its physical properties with those for other well-studied systems. BR CMi is an ellipsoidal variable seen under an intermediate orbital inclination of ∼51°, and it has an orbital period of 12.919059(15)d and a circular orbit. We used the disentangled component spectra to estimate the effective temperatures 9500(200) K and 4655(50) K by comparing them with model spectra. They correspond to spectral types B9.5e and G8III. We also used the disentangled spectra of both binary components as templates for the 2D cross-correlation to obtain accurate radial velocities and a reliable orbital solution. Some evidence of a secular period increase at a rate of (1.1±0.5) s per year was found. This, together with a very low mass ratio of 0.06 and a normal mass and radius of the mass gaining component, indicates that BR CMi is in a slow phase of the mass exchange after the mass-ratio reversal. It thus belongs to a still poorly populated subgroup of Be stars for which the origin of Balmer emission lines is safely explained as a consequence of mass transfer between the binary components.

Abstract Copyright:

Journal keyword(s): binaries: close - binaries: spectroscopic - stars: emission-line, Be - stars: individual: BR CMi (HD 61273) - stars: fundamental parameters

Simbad objects: 27

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Number of rows : 27

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 HD 232121 Al* 00 10 42.0679098681 +54 53 29.360355721   9.67       B5+K3III 172 0
2 V* RX Cas bL* 03 07 45.7481570255 +67 34 38.614798549   10.14 8.64     K1III+A5eIII 173 0
3 V* V617 Aur bL* 05 39 56.62399 +30 05 11.2366   8.86 8.15     F4III 37 1
4 HD 43246 SB* 06 16 22.1983433965 +28 51 07.132404490   7.82 7.41     A0Vn+F5III 42 0
5 V* HZ CMa Be* 06 50 23.3477914043 -31 42 21.807087882   5.829 5.747     B6IVe+A 81 0
6 HD 50846 Al* 06 54 54.7083961175 -01 22 32.849416553   8.46 8.43     B5/7Ib 134 0
7 HD 51956 SB* 06 59 31.7494034568 +00 55 00.357248267   8.31 7.51     F6Ib/II 33 0
8 * 1 CMi * 07 24 58.1797130190 +11 40 10.284327847   5.461 5.361     A5IV 40 0
9 HD 59059 * 07 28 47.2559346971 +15 06 35.365328104 6.06 6.17 6.22     B9IV 38 0
10 HD 59771 Em* 07 30 51.0696810014 -18 15 42.498127707   9.80 8.96     F2/3II 17 0
11 V* BR CMi a2* 07 38 50.9829375551 +07 57 59.645337369   7.36 7.15     B9.5+G8III 22 0
12 BD+08 1835 * 07 39 08.4549330604 +08 00 23.167587117   9.76 9.60     A2 1 0
13 HD 61341 * 07 39 09.6981095401 +07 49 51.425348774   8.16 7.96     A2 8 0
14 * bet Gem PM* 07 45 18.94987 +28 01 34.3160 3.00 2.14 1.14 0.39 -0.11 K0IIIb 1046 1
15 V* PW Pup bL* 07 49 06.0101460697 -31 07 42.620959488 10.54 10.23 9.53 9.85   G0Ie 37 0
16 V* UX Mon Al* 07 59 16.3751282592 -07 30 17.889948033   8.74 8.42     A2/3+G/K 124 0
17 V* TT Hya Al* 11 13 12.4975968306 -26 27 54.251048400   7.43 7.31     F0IV:kA2mA3:_sh 173 0
18 V* BY Cru bL* 12 04 48.6318277874 -62 00 08.191833660 7.85 8.18 7.63 8.70   F0Ib/II 34 0
19 HD 127208 Be* 14 30 40.4652158875 -22 27 39.314077664   7.12 6.96     B9IVe 32 0
20 * del Sco SB* 16 00 20.00528 -22 37 18.1431 1.30 2.20 2.32 2.36 2.49 B0.3IV 692 0
21 V* V393 Sco Al* 17 48 47.6025530213 -35 03 25.628506169   7.71 7.59     B3III 56 0
22 HD 174237 Be* 18 46 43.0889592280 +52 59 16.650319177 5.06 5.80 5.90     B3+F5III 190 0
23 * bet Lyr bL* 18 50 04.7952472 +33 21 45.609978 2.85 3.42 3.42 3.31 3.29 B8.5Ib-II 886 0
24 V* V448 Cyg bL* 20 06 09.9485954895 +35 23 09.614693894 7.89 8.45 8.16     O9.5V+B1Ib 141 0
25 HD 207739 SB* 21 49 58.8415737575 +43 57 56.833556720   9.22 8.59     kF0:mGepec 62 0
26 * 14 Lac bL* 22 50 21.7772135639 +41 57 12.179527815 5.49 5.961 5.910     B4+F9III 139 0
27 HD 218393 Be* 23 07 06.2120465053 +50 11 32.489137162 6.79 7.25 6.92     B3pe+K1III 143 0

    Equat.    Gal    SGal    Ecl

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2020.07.14-08:43:03

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