1SWASP J093010.78+533859.5

Quintuple star system in the constellation Ursa Major File:1SWASP J093010.78+533859.5 DSS.png J2000 Ursa MajorTIC 318210930 A 09 30 10.7410 +53 38 59.825 9.84 B 09 30 10.9127 +53 38 58.356 10.98 A K1V + K5V Algol B K3V + K3V W UMa A 12.24 0.17 78 3 78 pc ly number 3 pc ly number B −0.737 −12.997 14.2625 0.0165 Aa Ab 31.333 hours 5.762 0.010 solar radius 88.2 0.3 0 Ba Bb 5.465 hours 1.665 0.012 solar radius 86 4 0 J093010Aa 0.837 0.008 0.832 0.018 commas 5185 +25 −20 4.52 J093010Ab 0.674 0.007 0.669 0.018 commas 4325 +20 −15 4.62 y J093010Ba 0.86 0.02 0.79 0.04 commas 4700 50 4.58 0.261 0.012n1 J093010Bb 0.341 0.011 0.52 0.05 commas 4700 50 4.53 0.112 0.005n1 RX J0930.1+5339 J09302+5339 Simbad assigns the 1SWASP J093010.78+533859.5 designation to component B, but various sources make clear it applies to the whole "system" of four or five stars. Similarly, the designation 1SWASP J093012.84+533859.6 is also given to component B, but actually applies to an 18th-magnitude star 18" away. A V441 UMa 3807-759-1 B V442 UMa 3807-759-2 TIC+318210930 V441+UMa A V442+UMa B 1SWASP J093010.78+533859.5 (abbreviated as J093010), also known as V441 Ursae Majoris and V442 Ursae Majoris, is a quintuple star system located in the constellation Ursa Major. 10.1088/0004-6256/147/5/104 1SWASP J093010.78+533859.5: A Possible Hierarchical Quintuple System 2014 Koo Jae-Rim Lee Jae Woo Lee Byeong-Cheol Kim Seung-Lee Lee Chung-Uk Hong Kyeongsoo Lee Dong-Joo Rey Soo-Chang The Astronomical Journal 147 5 104 1402.4575 2014AJ....147..104KLohr M. E. Norton A. J. Gillen E. Busuttil R. June 12, 2015 The doubly eclipsing quintuple low-mass star system 1SWASP J093010.78+533859.5 Astronomy & Astrophysics 578 A103 10.1051/0004-6361/201525973 1504.07065 2015A&A...578A.103L The star system is located approximately 250 light-years from Earth, and was discovered using data from the "Super Wide Angle Search for Planets" (SuperWASP) project in the Canary Islands. Description 1SWASP J093010.78+533859.5 consists of two pairs of stars, designated J093010A and J093010B respectively, as well as a fifth star. The first pair of stars, J093010A, is a detached eclipsing binary (an Algol variable). The two stars within J093010A orbit with a period of about 1.3 days and are separated by about 5.8 solar radii. The second pair of stars, J093010B is a W Ursae Majoris variable; in this pair the two stars are so close as to be touching each other. The two stars within J093010B take about 5.5 hours (0.2277 days) to orbit each other.Gazeas K. July 2015 Disentangling the Quadruple System 1SWASP J093010.78+533859.5 Living Together: Planets 496 112 2015ASPC..496..112G The two pairs J093010A and J093010B are separated by about 1.89 arcseconds, so the separation between the two pairs is likely about 130 astronomical units. The fifth star was detected based on stationary spectral lines coming from the direction of 1SWASP J093010.78+533859.5. The fifth star likely orbits J093010A at a further distance than the eclipsing binary. Variability J093010A is a detached (Algol-type) eclipsing binary. Its magnitude drops from a maximum of 9.44 to a primary minimum of 9.75 and a secondary minimum of 9.58 every 1.31 days. It has been given the variable star designation V441 Ursae Majoris. J093010B is a contact (W UMa-type) eclipsing binary. Its magnitude drops by 0.28 magnitudes at the primary eclipse and 0.25 magnitudes during the secondary eclipse from a maximum magnitude of 10.55. The period is 0.23 days. It has been given the variable star designation V442 Ursae Majoris. yes center File:V441UMaLightCurve.png A light curve for V441 Ursae Majoris (J093010A), adapted from Lohr et al. (2015). The maximum brightness is the combined light of all 5 stars. File:V442UMaLightCurve.png A light curve for V442 Ursae Majoris (J093010B), adapted from Lohr et al. (2015). The maximum brightness is the combined light of all 5 stars. See also V1400 Centauri Notes n1 Calculated from absolute bolometric magnitude of 6.20 0.05 and 7.12 0.05 for J093010Ba and Bb, respectively, using the following formula: where L☉ is the Sun's bolometric luminosity, L★ is the star's bolometric luminosity, Mbol,☉ is the bolometric magnitude of the Sun, Mbol,★ is the bolometric magnitude of the star. References TIC+318210930 2025-07-07 V441+UMa 2025-07-07 V442+UMa 2025-07-07 1019985085615356672 1019985089906439040 2002A&A...384..180F The Tycho double star catalogue Fabricius C. Høg E. Makarov V. V. Mason B. D. Wycoff G. L. Urban S. E. Astronomy and Astrophysics 2002 384 180 10.1051/0004-6361:20011822 2017ARep...61...80S General catalogue of variable stars: Version GCVS 5.1 Samus' N. N. Kazarovets E. V. Durlevich O. V. Kireeva N. N. Pastukhova E. N. Astronomy Reports 2017 61 1 80 10.1134/S1063772917010085 Carroll, B. W. Ostlie, D. A. An Introduction to Modern Astrophysics https://archive.org/details/introductiontomo00bwca_613 limited 2nd Pearson 978-0-321-44284-0 60–62 2007 5 Category:Wide Angle Search for Planets Category:Ursa Major Category:Algol variables Category:W Ursae Majoris variables Ursae Majoris, V442 Category:K1V stars Category:K3V stars Category:K5V stars