2 Cassiopeiae

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2 Cassiopeiae
Cassiopeia constellation map.svg
Red circle.svg
Location of 2 Cassiopeiae (circled)
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Cassiopeia
Right ascension 23h 09m 44.1389s [1]
Declination +59° 19′ 57.687″ [1]
Apparent magnitude  (V)+5.679 [2]
Characteristics
Spectral type A4II [3] (kA5hA7mF0) [4]
U−B color index +0.31 [5]
B−V color index +0.33 [5]
Astrometry
Radial velocity (Rv)−13.58±0.15 [1]  km/s
Proper motion (μ)RA: +0.335 [1]   mas/yr
Dec.: +0.552 [1]   mas/yr
Parallax (π)1.1900 ± 0.0386  mas [1]
Distance 2,740 ± 90  ly
(840 ± 30  pc)
Absolute magnitude  (MV)−2.92 [6]
Details
Mass 5.3 [7]   M☉
Radius 41 [8]   R☉
Luminosity 3,014 [8]   L☉
Surface gravity (log g)1.93 [7]   cgs
Temperature 8,012 [9]   K
Metallicity [Fe/H]−0.23 [7]   dex
Rotational velocity (v sin i)5.3 [10]  km/s
Other designations
2  Cas, HR  8822, HD  218753, BD+58°2552, HIP  114365
Database references
SIMBAD data

2 Cassiopeiae (2 Cas) is a white bright giant in the constellation Cassiopeia, about 2,800 light years away. It is a chemically peculiar Am star.

2 Cassiopeiae has been described as an A4 type bright giant, but its spectrum is not easy to classify. The calcium K absorption lines indicate a hotter type than the hydrogen lines, while other metals indicate a cooler type, possibly as cool as F0. This makes it an Am star, a type of magnetic chemically peculiar star with unusual abundances showing in its spectrum due to chemical stratification in its atmosphere caused by slow rotation. [5]

About six times as massive as the Sun and 3,000 times as luminous, it has expanded away from the main sequence after exhausting its core hydrogen and now has an effective temperature of about 8,000  K . Some researchers have suggested that it is a post-AGB star. [3]

2 Cassiopeiae has a number of close companions listed in multiple star catalogues, [11] but none are thought to be gravitationally associated. [12]

Related Research Articles

<span class="mw-page-title-main">21 Aquilae</span> Star in the constellation Aquila

21 Aquilae is a solitary variable star in the equatorial constellation of Aquila. It has the variable star designation V1288 Aql; 21 Aquilae is its Flamsteed designation. This object is visible to the naked eye as a dim, blue-white hued star with a baseline apparent visual magnitude of about 5.1. The star is located at a distance of around 680 light-years from Earth, give or take a 20 light-year margin of error. It is moving closer to the Earth with a heliocentric radial velocity of –5 km/s.

38 Boötis is a single star in the northern constellation of Boötes, located approximately 157 light years from the Sun. It has the traditional name Merga and the Bayer designation h Boötis; 38 Boötis is the star's Flamsteed designation. This object is visible to the naked eye as a dim, yellow-white hued star with an apparent visual magnitude of 5.76. It is moving closer to the Earth with a heliocentric radial velocity of −4.5 km/s.

<span class="mw-page-title-main">Mu Cassiopeiae</span>

Mu Cassiopeiae, Latinized from μ Cassiopeiae, is a binary star system in the constellation Cassiopeia. This system shares the name Marfak with Theta Cassiopeiae, and the name was from Al Marfik or Al Mirfaq (المرفق), meaning "the elbow". It is dimly visible to the naked eye as a point of light with an apparent visual magnitude of 5.16. The system is located at a distance of 25 light years from the Sun based on parallax, and is moving closer with a high radial velocity of −98 km/s. This star will move into the constellation Perseus around 5200 AD.

<span class="mw-page-title-main">HR 511</span> Star in the constellation Cassiopeia

HR 511 is an orange dwarf of spectral type K0V in the constellation Cassiopeia. With an apparent magnitude of 5.63, it is faintly visible to the naked eye. The star is relatively close, 32.8 light years from the Sun.

<span class="mw-page-title-main">V337 Carinae</span> Star in the constellation of Carina

V337 Carinae is a K-type bright giant star in the constellation of Carina. It is an irregular variable and has an apparent visual magnitude which varies between 3.36 and 3.44.

<span class="mw-page-title-main">Kappa Cassiopeiae</span> Star in the constellation Cassiopeia

Kappa Cassiopeiae is a star in the constellation Cassiopeia.

<span class="mw-page-title-main">Pi Cassiopeiae</span> Variable star in the constellation Cassiopeia

Pi Cassiopeiae, Latinized from π Cassiopeiae, is a close binary star system in the constellation Cassiopeia. It is visible to the naked eye with an apparent visual magnitude of +4.949. Based upon an annual parallax shift of 18.63 mas as seen from Earth, this system is located about 175 light years from the Sun.

<span class="mw-page-title-main">4 Cassiopeiae</span> Star in the constellation Cassiopeia

4 Cassiopeiae is a red giant in the northern constellation of Cassiopeia, located approximately 790 light-years away from the Sun. It is visible to the naked eye as a faint, red-hued star with a baseline apparent visual magnitude of 4.96. At the distance of this system, its visual magnitude is diminished by an extinction of 0.56 due to interstellar dust. This system is moving closer to the Earth with a heliocentric radial velocity of −39 km/s.

<span class="mw-page-title-main">Omega Cassiopeiae</span> Binary star system in constellation Cassiopeia

Omega Cassiopeiae is a binary star system in the northern constellation of Cassiopeia. It has a combined apparent visual magnitude of +4.99, which means it is a faint star but visible to the naked eye. Based upon an annual parallax shift of 4.65 mas as seen from Earth, this system is located roughly 730 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction of 0.16 due to interstellar dust.

<span class="mw-page-title-main">Theta Persei</span> Star system in the constellation Perseus

Theta Persei is a star system 37 light years away from Earth, in the constellation Perseus. It is one of the closest naked-eye stars.

HD 7853 is a double star in the constellation Andromeda. With an apparent magnitude of 6.46, it can barely be seen with the naked eye even on the best of nights. The system is located approximately 130 parsecs (420 ly) distant, and the brighter star is an Am star, meaning that it has unusual metallic absorption lines. The spectral classification of kA5hF1mF2 means that it would have a spectral class of A5 if it were based solely on the calcium K line, F2 if based on the lines of other metals, and F1 if based on the hydrogen absorption lines. The two components are six arc-seconds apart and the secondary is three magnitudes fainter than the primary.

<span class="mw-page-title-main">1 Serpentis</span> Red giant star in the constellation Virgo

1 Serpentis is a red giant in the constellation Virgo with an apparent magnitude of 5.5. It is a red clump giant, a cool horizontal branch star that is fusing helium in its core. It has expanded to over 13 times the radius of the Sun and although it is cooler at 4,581 K it is 77 times more luminous. It is 322 light years away.

HD 102350 is a single star in the constellation Centaurus. It has a yellow hue and is visible to the naked eye with an apparent visual magnitude of 4.11. The distance to this star is approximately 390 light years based on parallax, but it is drifting closer with a radial velocity of −3 km/s. It has an absolute magnitude of −1.51.

<span class="mw-page-title-main">V1073 Scorpii</span> Variable star in the constellation Scorpius

V1073 Scorpii is a variable star in the constellation Scorpius. It has a non-Greek Bayer designation of k Scorpii. The star has a blue-white hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around +4.87. Parallax measurements yield a distance estimate of approximately 2,920 ly (896 pc) from the Sun, and it is drifting further away with a radial velocity of +7 km/s. It has an absolute magnitude of −6.8

Psi2 Draconis is a solitary giant star in the northern circumpolar constellation of Draco, also designated 34 Draconis. It lies just over a degree east of the brighter Psi1 Draconis. Psi2 Draconis has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.45. It is located at a distance of 940 light-years from the Sun based on parallax, but is drifting closer with a radial velocity of −2 km/s.

Eta Microscopii, Latinised as η Microscopii, is a solitary star in the constellation Microscopium. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.53. The star is located around 910 light-years distant from the Sun based on parallax, and is drifting further away with a radial velocity of +22 km/s.

<span class="mw-page-title-main">S Cassiopeiae</span> Star in the constellation Cassiopeia

S Cassiopeiae is a Mira variable and S-type star in the constellation Cassiopeia. It is an unusually cool star, rapidly losing mass and surrounded by dense gas and dust producing masers.

<span class="mw-page-title-main">BO Carinae</span> Star in the constellation Carina

BO Carinae, also known as HD 93420, is an irregular variable star in the constellation Carina.

HD 200044 is a solitary star in the equatorial constellation Delphinus. It has an apparent magnitude of 5.7, allowing it to be faintly seen with the naked eye. The object is located 598 light years away, but is approaching the Solar System with a heliocentric radial velocity of −15.07 km/s.

<span class="mw-page-title-main">9 Cassiopeiae</span> Star in the constellation Cassiopeia

9 Cassiopeiae is a white giant star in the constellation Cassiopeia, about 2,370 light years away.

References

  1. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  2. ↑ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode:2000A&A...355L..27H. doi:10.1888/0333750888/2862.
  3. 1 2 Gray, R. O.; Napier, M. G.; Winkler, L. I. (2001). "The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. I. Precise Spectral Types for 372 Stars". The Astronomical Journal. 121 (4): 2148. Bibcode:2001AJ....121.2148G. doi: 10.1086/319956 .
  4. ↑ Abt, Helmut A.; Morrell, Nidia I. (1995). "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars". Astrophysical Journal Supplement. 99: 135. Bibcode:1995ApJS...99..135A. doi: 10.1086/192182 .
  5. 1 2 3 Renson, P.; Manfroid, J. (May 2009). "Catalogue of Ap, HgMn and Am stars". Astronomy and Astrophysics. 498 (3): 961–966. Bibcode:2009A&A...498..961R. doi: 10.1051/0004-6361/200810788 .
  6. ↑ Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN   1562-6873. ISSN   1063-7737. S2CID   119257644.
  7. 1 2 3 Anders, F.; Khalatyan, A.; Chiappini, C.; Queiroz, A. B.; Santiago, B. X.; Jordi, C.; Girardi, L.; Brown, A. G. A.; Matijevič, G.; Monari, G.; Cantat-Gaudin, T.; Weiler, M.; Khan, S.; Miglio, A.; Carrillo, I.; Romero-Gómez, M.; Minchev, I.; De Jong, R. S.; Antoja, T.; Ramos, P.; Steinmetz, M.; Enke, H. (2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy and Astrophysics. 628: A94. arXiv: 1904.11302 . Bibcode:2019A&A...628A..94A. doi:10.1051/0004-6361/201935765. S2CID   131780028.
  8. 1 2 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  9. ↑ Stassun, Keivan G.; et al. (2019-10-01). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv: 1905.10694 . Bibcode:2019AJ....158..138S. doi: 10.3847/1538-3881/ab3467 . hdl: 1721.1/124721 . ISSN   0004-6256. S2CID   166227927.
  10. ↑ Schröder, C.; Reiners, Ansgar; Schmitt, Jürgen H. M. M. (January 2009). "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo". Astronomy and Astrophysics. 493 (3): 1099–1107. Bibcode:2009A&A...493.1099S. doi: 10.1051/0004-6361:200810377 .
  11. ↑ Mason, Brian D.; et al. (December 2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466–3471. Bibcode:2001AJ....122.3466M. doi: 10.1086/323920 .
  12. ↑ Eggleton, P. P.; Tokovinin, A. A. (3 September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society . 389 (2): 869–879. arXiv: 0806.2878 . Bibcode:2008MNRAS.389..869E. doi: 10.1111/j.1365-2966.2008.13596.x . S2CID   14878976.
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