The Open UniversitySkip to content
 

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 González, E. (2015). The doubly eclipsing quintuple low-mass star system 1SWASP J093010.78+533859.5. Astronomy & Astrophysics, 578, article no. A103.

Full text available as:
[img]
Preview
PDF (Version of Record) - Requires a PDF viewer such as GSview, Xpdf or Adobe Acrobat Reader
Download (2MB) | Preview
DOI (Digital Object Identifier) Link: https://doi.org/10.1051/0004-6361/201525973
Google Scholar: Look up in Google Scholar

Abstract

Our discovery of 1SWASP J093010.78+533859.5 as a probable doubly eclipsing quadruple system, containing a contact binary with P ~ 0.23 d and a detached binary with P ~ 1.31 d, 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+25-20 and 4325+20-15 K, 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 −12 km s-1, which match the average radial velocity of the fifth star; consistent distance estimates for both subsystems of d = 78 ± 3 and d = 73 ± 4 pc are also found, and, with some further assumptions, of d = 83 ± 9 pc 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.

Item Type: Journal Item
Copyright Holders: 2015 ESO
ISSN: 1432-0746
Project Funding Details:
Funded Project NameProject IDFunding Body
PhD StudentshipNot SetSTFC/OU
Consolidated Grant (post-doc position with Simon Clark)Not SetSTFC
Keywords: stars - individual - 1SWASP J093010.78+533859.5; binaries - close; binaries -eclipsing; binaries - spectroscopic; multiple star systems; archival research
Academic Unit/School: Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
Item ID: 43484
Depositing User: Marcus Lohr
Date Deposited: 18 Jun 2015 10:12
Last Modified: 09 Dec 2018 06:11
URI: http://oro.open.ac.uk/id/eprint/43484
Share this page:

Metrics

Altmetrics from Altmetric

Citations from Dimensions

Download history for this item

These details should be considered as only a guide to the number of downloads performed manually. Algorithmic methods have been applied in an attempt to remove automated downloads from the displayed statistics but no guarantee can be made as to the accuracy of the figures.

Actions (login may be required)

Policies | Disclaimer

© The Open University   contact the OU