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Iota Cassiopeiae

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Variable star in the constellation Cassiopeiae
ι Cassiopeiae

The Bayer-designated stars in Cassiopeia. Iota Cassiopeiae is circled.
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cassiopeia
ι Cas A
Right ascension 02 29 03.960
Declination +67° 24′ 08.70″
Apparent magnitude (V) 4.61 (4.65 / 8.48)
ι Cas B
Right ascension 02 29 03.567
Declination +67° 24′ 07.01″
Apparent magnitude (V) 6.87
ι Cas C
Right ascension 02 29 05.086
Declination +67° 24′ 05.53″
Apparent magnitude (V) 9.05 (9.14 / 11.84)
Characteristics
U−B color index +0.03
B−V color index +0.12
ι Cas A
Spectral type A3p / G6
Variable type α CVn
ι Cas B
Spectral type F5
ι Cas C
Spectral type K4 / M2
U−B color index +0.18
B−V color index +0.72
Astrometry
Radial velocity (Rv)1.2 ± 2 km/s
Proper motion (μ) RA: -26.61 mas/yr
Dec.: 38.21 mas/yr
Parallax (π)22.22 ± 0.08 mas
Distance146.8 ± 0.5 ly
(45.0 ± 0.2 pc)
Absolute magnitude (MV)1.62 ± 0.07 (Aa)
5.60 ± 0.17 (Ab)
Orbit
Primaryι Cas Aa
Companionι Cas Ab
Period (P)48.72 ± 0.45 yr
Semi-major axis (a)0.423 ± 0.004″
Eccentricity (e)0.637 ± 0.004
Inclination (i)148.2 ± 1.3°
Longitude of the node (Ω)176.6 ± 1.8°
Periastron epoch (T)B 1993.21 ± 0.05
Argument of periastron (ω)
(secondary)
328.2 ± 1.9°
Orbit
Primaryι Cas A
Companionι Cas B
Period (P)2400 yr
Semi-major axis (a)6.50″
Eccentricity (e)0.40
Inclination (i)102.9 ± 0.3°
Longitude of the node (Ω)188.0 ± 0.9°
Periastron epoch (T)B 940 ± 47
Argument of periastron (ω)
(secondary)
113.3 ± 3.4°
Details
ι Cas Aa
Mass1.98 M
Radius2.3 ± 0.4 R
Luminosity24 L
Temperature8360 ± 275 K
Rotation1.74033 d
Rotational velocity (v sin i)48 km/s
Age100 Myr
ι Cas Ab
Mass0.98 M
ι Cas B
Mass1.28 M
Temperature6540 K
ι Cas Ca
Temperature4520 ± 20 K
ι Cas Cb
Temperature3590 ± 45 K
Other designations
BD+66° 213, HD 15089, HIP 11569, HR 707, SAO 12298
ι Cas A: TYC 4058-1504-1
ι Cas B: TYC 4058-1504-2
ι Cas C: TYC 4058-1505-1
Database references
ι Cas AB
ι Cas A
ι Cas B
ι Cas C

Iota Cassiopeiae (ι Cas, ι Cassiopeiae) is a star system in the constellation Cassiopeia. The system has a combined apparent magnitude of 4.53, making it visible to the naked eye. Based on its parallax, it is located about 133 light-years (41 parsecs) from Earth.

Components

A light curve for Iota Cassiopeiae, plotted from TESS data

Iota Cassiopeiae is known to be a quintuple star system. The brightest star system, ι Cassiopeiae A, contains a white-colored A-type main-sequence star with a mean apparent magnitude of +4.61. The primary is itself a tighter binary star system. The two stars were resolved by adaptive optics. These are designated Aa and Ab (although confusingly they may also be labeled as A and Aa, respectively). The primary is classified as an Alpha Canum Venaticorum-type variable star and the brightness of the system varies from magnitude +4.45 to +4.53 with a period of 1.74 days, because of its magnetic field. The variability in brightness was first detected by Karl D. Rakos in 1962, although its spectrum was known to be variable from earlier observations. The fainter companion is a G-type star with a mass of 0.98 M. The orbital period of the system is about 49 years.

ι Cassiopeiae B is a yellow-white F-type main sequence dwarf with an apparent magnitude of +6.87. It orbits around ι Cassiopeiae A approximately every 2,400 years with a semi-major axis of around 6.5 arcseconds, but the orbit is not very well constrained. This object may be causing Kozai–Lidov cycles in the inner orbital pair.

ι Cassiopeiae C is itself another binary, designated Ca and Cb, or just C and c. It comprises two stars, a K-type star and an M-type star. It is currently at an angular distance of about 7 arcseconds from the AB pair. Since the semimajor axis of the AB orbit is about 6.5 arcseconds, the true semimajor axis of C's orbit around them is thought to be significantly larger than 7 arcseconds.

References

  1. ^ Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27 – L30. Bibcode:2000A&A...355L..27H.
  2. ^ Drummond, Jack; Milster, Scott; Ryan, Patrick; Roberts, Jr., Lewis C. (2003). "ι Cassiopeiae: Orbit, Masses, and Photometry from Adaptive Optics Imaging in the I and H Bands". The Astrophysical Journal. 585 (2): 1007. Bibcode:2003ApJ...585.1007D. doi:10.1086/346224.
  3. ^ Christou, Julian C.; Drummond, Jack D. (2006). "Measurements of Binary Stars, Including Two New Discoveries, with the Lick Observatory Adaptive Optics System". The Astronomical Journal. 131 (6): 3100. Bibcode:2006AJ....131.3100C. doi:10.1086/503255.
  4. ^ Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
  5. ^ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  6. Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Washington. Bibcode:1953GCRV..C......0W.
  7. ^ van Leeuwen, F.; et al. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  8. ^ Tokovinin, A. (2021). "Inner and Outer Orbits in 13 Resolved Hierarchical Stellar Systems". The Astronomical Journal. 161 (3): 144. arXiv:2101.02976. Bibcode:2021AJ....161..144T. doi:10.3847/1538-3881/abda42. S2CID 231419112.
  9. ^ De Rosa, R. J.; Patience, J.; Vigan, A.; Wilson, P. A.; Schneider, A.; McConnell, N. J.; Wiktorowicz, S. J.; Marois, C.; Song, I.; MacIntosh, B.; Graham, J. R.; Bessell, M. S.; Doyon, R.; Lai, O. (2012). "The Volume-limited A-Star (VAST) survey - II. Orbital motion monitoring of A-type star multiples". Monthly Notices of the Royal Astronomical Society. 422 (4): 2765. arXiv:1112.3666. Bibcode:2012MNRAS.422.2765D. doi:10.1111/j.1365-2966.2011.20397.x. S2CID 102487103.
  10. ^ Aurière, M.; Wade, G. A.; Silvester, J.; Lignières, F.; Bagnulo, S.; Bale, K.; Dintrans, B.; Donati, J. F.; Folsom, C. P.; Gruberbauer, M.; Hui Bon Hoa, A.; Jeffers, S.; Johnson, N.; Landstreet, J. D.; Lèbre, A.; Lueftinger, T.; Marsden, S.; Mouillet, D.; Naseri, S.; Paletou, F.; Petit, P.; Power, J.; Rincon, F.; Strasser, S.; Toqué, N. (2007). "Weak magnetic fields in Ap/Bp stars". Astronomy and Astrophysics. 475 (3): 1053. arXiv:0710.1554. Bibcode:2007A&A...475.1053A. doi:10.1051/0004-6361:20078189. S2CID 54850596.
  11. "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  12. Rakos, Karl D. (1962). "Photoelectric investigation of magnetic and spectrum variable stars". Bulletin / Lowell Observatory. 5 (12): 227–256. Bibcode:1962LowOB...5..227R. Retrieved 10 October 2024.
  13. Tokovinin, A. A. (1997). "MSC - a catalogue of physical multiple stars". Astronomy and Astrophysics Supplement Series. 124: 75–84. Bibcode:1997A&AS..124...75T. doi:10.1051/aas:1997181. (HR 707 Archived 2021-02-05 at the Wayback Machine)
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