2015A&A...578A.103L


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.11CET04:44:25

2015A&A...578A.103L - Astronomy and Astrophysics, volume 578A, 103-103 (2015/6-1)

The doubly eclipsing quintuple low-mass star system 1SWASP J093010.78+533859.5.

LOHR M.E., NORTON A.J., GILLEN E., BUSUTTIL R., KOLB U.C., AIGRAIN S., McQUILLAN A., HODGKIN S.T. and GONZALEZ E.

Abstract (from CDS):

Our discovery of 1SWASP J093010.78+533859.5 as a probable doubly eclipsing quadruple system, containing a contact binary with P∼0.23d and a detached binary with P∼1.31d, was announced in 2013. Subsequently, Koo and collaborators confirmed the detached binary spectroscopically, and identified a fifth set of static spectral lines at its location, corresponding to an additional non-eclipsing component of the system. Here we present new spectroscopic and photometric observations, allowing confirmation of the contact binary and improved modelling of all four eclipsing components. The detached binary is found to contain components of masses 0.837±0.008 and 0.674±0.007M, with radii of 0.832±0.018 and 0.669±0.018R and effective temperatures of 5185–20+25 and 4325–15+20K, respectively; the contact system has masses 0.86±0.02 and 0.341±0.011M, radii of 0.79±0.04 and 0.52±0.05R, respectively, and a common effective temperature of 4700±50 K. The fifth star is of similar temperature and spectral type to the primaries in the two binaries. Long-term photometric observations indicate the presence of a spot on one component of the detached binary, moving at an apparent rate of approximately one rotation every two years. Both binaries have consistent system velocities around -11 to -12km/s, which match the average radial velocity of the fifth star; consistent distance estimates for both subsystems of d=78±3 and d=73±4pc are also found, and, with some further assumptions, of d=83±9pc for the fifth star. These findings strongly support the claim that both binaries - and very probably all five stars - are gravitationally bound in a single system. The consistent angles of inclination found for the two binaries (88.2±0.3° and 86±4°) may also indicate that they originally formed by fragmentation (around 9-10 Gyr ago) from a single protostellar disk, and subsequently remained in the same orbital plane.

Abstract Copyright:

Journal keyword(s): stars: individual: 1SWASP J093010.78+533859.5 - binaries: close - binaries: eclipsing - binaries: spectroscopic

Simbad objects: 13

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Number of rows : 13

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 OGLE LMC-ECL-16545 EB* 05 28 09.27 -70 12 56.0     19.832   19.416 ~ 3 0
2 NAME Cze V343 EB* 05 48 24.0129958401 +30 57 03.577649865   14.07 13.68 13.71   ~ 9 0
3 TYC 3807-1503-1 * 09 29 23.4438082395 +53 31 12.144770717   11.37 10.94     ~ 2 0
4 GSC 03807-00759 ** 09 30 10.770144 +53 38 59.63712   10.52 9.54 9.28   ~ 22 0
5 TYC 3807-759-2 WU* 09 30 10.9127422293 +53 38 58.359514124   11.84 10.98     K3V+K3V 4 0
6 TYC 3807-54-1 PM* 09 30 13.9303790515 +53 31 06.213161276   10.45 9.96     ~ 3 0
7 TYC 3807-621-1 * 09 30 23.5417184167 +53 28 51.857882541   11.42 10.86     ~ 1 0
8 TYC 3807-1509-1 * 09 30 43.1971418402 +53 36 44.417566135   11.18 10.59     ~ 2 0
9 [MMN2007] A1 gLS 14 17 35.9 +52 26 46     21.53   19.69 ~ 76 0
10 V* BW Dra WU* 15 11 50.0992475613 +61 51 41.230539303   9.39   8.3   B0 114 2
11 V* BV Dra WU* 15 11 50.3595172449 +61 51 25.282913496   8.54   7.7   F9V+F8V 141 2
12 V* V994 Her Al* 18 27 45.89332 +24 41 50.6652   7.14 7.14     B9V 47 1
13 KOI-28 Al* 19 08 39.5630399563 +39 22 36.980792633   12.82 11.58     ~ 37 0

    Equat.    Gal    SGal    Ecl

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2019.12.11-04:44:25

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