Astronomy:1SWASP J093010.78+533859.5

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Short description: Quintuple star system in the constellation Ursa Major
1SWASP J093010.78+533859.5
Observation data
{{#ifeq:J2000|J2000.0 (ICRS)|Epoch J2000.0      Equinox J2000.0 (ICRS)| Epoch J2000      [[Astronomy:Equinox (celestial coordinates)|Equinox J2000}}
Constellation Ursa Major[1]
A
Right ascension  09h 30m 10.7410s[2]
Declination +53° 38′ 59.825″[2]
Apparent magnitude (V) 9.84[3]
B
Right ascension  09h 30m 10.9127s[4]
Declination +53° 38′ 58.356″[4]
Apparent magnitude (V) 10.98[3]
Characteristics
A
Spectral type K1V + K5V[5]
Variable type Algol[6]
B
Spectral type K3V + K3V[5]
Variable type W UMa[6]
Astrometry
A
Radial velocity (Rv)12.24±0.17[7] km/s
Distance250±9.8 ly
(78±3 pc)
B
Proper motion (μ) RA: −0.737[4] mas/yr
Dec.: −12.997[4] mas/yr
Parallax (π)14.2625 ± 0.0165[4] mas
Distance228.7 ± 0.3 ly
(70.11 ± 0.08 pc){{{dist_ly2}}} ly
Orbit[7]
PrimaryAa
CompanionAb
Period (P)31.333 hours
Semi-major axis (a)5.762±0.010 R☉
Eccentricity (e)0
Inclination (i)88.2±0.3°
Orbit[7]
PrimaryBa
CompanionBb
Period (P)5.465 hours
Semi-major axis (a)1.665±0.012 R☉
Eccentricity (e)0
Inclination (i)86±4°
Details[7]
J093010Aa
Mass0.837±0.008 M☉
Radius0.832±0.018 R☉
Surface gravity (log g)4.52 cgs
Temperature5,185+25
−20 K
J093010Ab
Mass0.674±0.007 M☉
Radius0.669±0.018 R☉
Surface gravity (log g)4.62 cgs
Temperature4,325+20
−15 K
J093010Ba
Mass0.86±0.02 M☉
Radius0.79±0.04 R☉
Luminosity0.261±0.012[lower-alpha 1] L☉
Surface gravity (log g)4.58 cgs
Temperature4,700±50 K
J093010Bb
Mass0.341±0.011 M☉
Radius0.52±0.05 R☉
Luminosity0.112±0.005[lower-alpha 1] L☉
Surface gravity (log g)4.53 cgs
Temperature4,700±50 K
Other designations
RX J0930.1+5339, WDS J09302+5339[8][lower-alpha 2]
A: V441 UMa, TYC 3807-759-1[9]
B: V442 UMa, TYC 3807-759-2[10]
Database references
SIMBADdata
A
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.[5][7] The star system is located approximately 250 light-years from Earth,[7] 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.[7] 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.[6]

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.[5]

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.[11]

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.[11]

  • A light curve for V441 Ursae Majoris (J093010A), adapted from Lohr et al. (2015).[7] The maximum brightness is the combined light of all 5 stars.
    A light curve for V441 Ursae Majoris (J093010A), adapted from Lohr et al. (2015).[7] The maximum brightness is the combined light of all 5 stars.
  • A light curve for V442 Ursae Majoris (J093010B), adapted from Lohr et al. (2015).[7] The maximum brightness is the combined light of all 5 stars.
    A light curve for V442 Ursae Majoris (J093010B), adapted from Lohr et al. (2015).[7] The maximum brightness is the combined light of all 5 stars.

See also

Notes

  1. ↑ 1.0 1.1 Calculated from absolute bolometric magnitude of 6.20±0.05 and 7.12±0.05 for J093010Ba and Bb, respectively,[7] using the following formula:[12] L⋆L⊙=100.4(Mbol,⊙−Mbol,⋆) 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.
  2. ↑ 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.[7][5] Similarly, the designation 1SWASP J093012.84+533859.6 is also given to component B, but actually applies to an 18th-magnitude star 18" away.[7]

References

  1. ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific 99 (617): 695. doi:10.1086/132034. Bibcode: 1987PASP...99..695R  Constellation record for this object at VizieR.
  2. ↑ 2.0 2.1 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  3. ↑ 3.0 3.1 Fabricius, C.; Høg, E.; Makarov, V. V.; Mason, B. D.; Wycoff, G. L.; Urban, S. E. (2002). "The Tycho double star catalogue". Astronomy and Astrophysics 384: 180. doi:10.1051/0004-6361:20011822. Bibcode: 2002A&A...384..180F. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  5. ↑ 5.0 5.1 5.2 5.3 5.4 Koo, Jae-Rim; Lee, Jae Woo; Lee, Byeong-Cheol; Kim, Seung-Lee; Lee, Chung-Uk; Hong, Kyeongsoo; Lee, Dong-Joo; Rey, Soo-Chang (2014). "1SWASP J093010.78+533859.5: A Possible Hierarchical Quintuple System". The Astronomical Journal 147 (5): 104. doi:10.1088/0004-6256/147/5/104. Bibcode: 2014AJ....147..104K. 
  6. ↑ 6.0 6.1 6.2 Gazeas, K. (July 2015). "Disentangling the Quadruple System 1SWASP J093010.78+533859.5". Living Together: Planets 496: 112. Bibcode: 2015ASPC..496..112G. 
  7. ↑ 7.00 7.01 7.02 7.03 7.04 7.05 7.06 7.07 7.08 7.09 7.10 7.11 Lohr, 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. doi:10.1051/0004-6361/201525973. Bibcode: 2015A&A...578A.103L. 
  8. ↑ "TIC+318210930". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=TIC%2B318210930. 
  9. ↑ "V441+UMa". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V441%2BUMa. 
  10. ↑ "V442+UMa". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V442%2BUMa. 
  11. ↑ 11.0 11.1 Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports 61 (1): 80. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S. 
  12. ↑ Carroll, B. W.; Ostlie, D. A. (2007). An Introduction to Modern Astrophysics (2nd ed.). Pearson. pp. 60–62. ISBN 978-0-321-44284-0. https://archive.org/details/introductiontomo00bwca_613. 



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