4 Cassiopeiae: Difference between revisions
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'''4 Cassiopeiae''' is a wide [[binary star]]<ref name=Eggleton2008/> system in the northern [[constellation]] of [[Cassiopeia (constellation)|Cassiopeia]],<ref name=SIMBAD/> located approximately 790 [[light-year]]s away from the Sun.<ref name=vanLeeuwen2007/> It is visible to the naked eye as a faint, red-hued star with a baseline [[apparent visual magnitude]] of 4.96.<ref name=Anderson2012/> At the distance of this system, its visual magnitude is diminished by an [[extinction (astronomy)|extinction]] of 0.56 due to [[interstellar dust]].<ref name=Famaey2005/> This system is moving closer to the Earth with a heliocentric [[radial velocity]] of −39 km/s.<ref name=Famaey2009/> |
'''4 Cassiopeiae''' is a wide [[binary star]]<ref name=Eggleton2008/> system in the northern [[constellation]] of [[Cassiopeia (constellation)|Cassiopeia]],<ref name=SIMBAD/> located approximately 790 [[light-year]]s away from the Sun.<ref name=vanLeeuwen2007/> It is visible to the naked eye as a faint, red-hued star with a baseline [[apparent visual magnitude]] of 4.96.<ref name=Anderson2012/> At the distance of this system, its visual magnitude is diminished by an [[extinction (astronomy)|extinction]] of 0.56 due to [[interstellar dust]].<ref name=Famaey2005/> This system is moving closer to the Earth with a heliocentric [[radial velocity]] of −39 km/s.<ref name=Famaey2009/> |
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The primary member of this system, component A, is an [[stellar evolution|evolved]] [[red giant]] star, currently on the [[asymptotic giant branch]],<ref name=eggen1992/> with a [[stellar classification]] of M2− IIIab.<ref name=Anderson2012/> It is a suspected [[variable star]] of unknown type with a brightness that varies from visual magnitude 4.95 down to 5.00.<ref name=gcvs2017/> As of 2011, the magnitude 9.88 secondary, component B, lay at an [[angular separation]] of {{Val|96.10|ul=arcsecond}} along a [[position angle]] of 226° relative to the primary.<ref name=WDSC2014/> |
The primary member of this system, component A, is an [[stellar evolution|evolved]] [[red giant]] star, currently on the [[asymptotic giant branch]],<ref name=eggen1992/> with a [[stellar classification]] of M2− IIIab.<ref name=Anderson2012/> It is a suspected [[variable star]] of unknown type with a brightness that varies from visual magnitude 4.95 down to 5.00.<ref name=gcvs2017/> As of 2011, the magnitude 9.88 secondary, component B, lay at an [[angular separation]] of {{Val|96.10|ul=arcsecond}} along a [[position angle]] of 226° relative to the primary.<ref name=WDSC2014/> |
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4 Cassiopeiae is 40' north of the [[open cluster]] [[Messier 52]], near the constellation border with [[Cepheus (constellation)|Cepheus]], although it is not a member of the cluster.<ref name=baumgardt2000/> |
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==References== |
==References== |
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<ref name=SIMBAD>{{cite simbad | title=4 Cas | access-date=2019-04-13 }}</ref> |
<ref name=SIMBAD>{{cite simbad | title=4 Cas | access-date=2019-04-13 }}</ref> |
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<ref name=baumgardt2000>{{cite journal |bibcode=2000A&AS..146..251B |title=Absolute proper motions of open clusters. I. Observational data |last1=Baumgardt |first1=H. |last2=Dettbarn |first2=C. |last3=Wielen |first3=R. |journal=Astronomy and Astrophysics Supplement Series |year=2000 |volume=146 |issue=2 |page=251 |doi=10.1051/aas:2000362 |arxiv=astro-ph/0010306 |s2cid=7180188 }}</ref> |
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<ref name="Koen">{{cite journal |
<ref name="Koen">{{cite journal |
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Revision as of 13:42, 4 October 2022
 A light curve for 4 Cassiopeiae, plotted from Hipparcos data.[1] The assumed period is from Koen and Eyer (2002).[2] | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Cassiopeia |
| Right ascension | 23h 24m 50.26237s[3] |
| Declination | +62° 16′ 58.1094″[3] |
| Apparent magnitude (V) | 4.96[4] (4.95–5.00)[5] |
| Characteristics | |
| Evolutionary stage | AGB[6] |
| Spectral type | M2− IIIab[4] |
| B−V color index | 1.676±0.010[4] |
| Variable type | suspected[5] |
| Astrometry | |
| Radial velocity (Rv) | −38.99±0.23[7] km/s |
| Proper motion (μ) | RA: +12.29[3] mas/yr Dec.: −12.44[3] mas/yr |
| Parallax (π) | 4.15 ± 0.21 mas[3] |
| Distance | 790 ± 40 ly (240 ± 10 pc) |
| Absolute magnitude (MV) | −1.94[4] |
| Details | |
| Radius | 54[8] R☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
.jpg)
4 Cassiopeiae is a wide binary star[10] system in the northern constellation of Cassiopeia,[9] located approximately 790 light-years away from the Sun.[3] It is visible to the naked eye as a faint, red-hued star with a baseline apparent visual magnitude of 4.96.[4] At the distance of this system, its visual magnitude is diminished by an extinction of 0.56 due to interstellar dust.[11] This system is moving closer to the Earth with a heliocentric radial velocity of −39 km/s.[7]
The primary member of this system, component A, is an evolved red giant star, currently on the asymptotic giant branch,[6] with a stellar classification of M2− IIIab.[4] It is a suspected variable star of unknown type with a brightness that varies from visual magnitude 4.95 down to 5.00.[5] As of 2011, the magnitude 9.88 secondary, component B, lay at an angular separation of 96.10″ along a position angle of 226° relative to the primary.[12]
4 Cassiopeiae is 40' north of the open cluster Messier 52, near the constellation border with Cepheus, although it is not a member of the cluster.[13]
References
- ^ "Light Curve", Hipparcos ESA, ESA, retrieved 3 October 2022.
- ^ Koen, Chris; Eyer, Laurent (March 2002). "New periodic variables from the Hipparcos epoch photometry". Monthly Notices of the Royal Astronomical Society. 331 (1): 45–59. Bibcode:2002MNRAS.331...45K. doi:10.1046/j.1365-8711.2002.05150.x. Retrieved 4 October 2022.
- ^ a b c d e f van Leeuwen, F. (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.
- ^ a b c d e f Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
- ^ a b c Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017), "General catalogue of variable stars", Astronomy Reports, 5.1, 61 (1): 80, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
- ^ a b Eggen, O. J. (1992), "Asymptotic giant branch stars near the sun", The Astronomical Journal, 104: 275, Bibcode:1992AJ....104..275E, doi:10.1086/116239.
- ^ a b Famaey, B.; et al. (2009), "Spectroscopic binaries among Hipparcos M giants. I. Data, orbits, and intrinsic variations", Astronomy and Astrophysics, 498 (2): 627–640, arXiv:0901.0934, Bibcode:2009A&A...498..627F, doi:10.1051/0004-6361/200810698, S2CID 18739721.
- ^ Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics, 367 (2) (Third ed.): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
- ^ a b "4 Cas". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-13.
- ^ Eggleton, P. P.; Tokovinin, A. A. (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.
- ^ Famaey, B.; et al. (January 2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters", Astronomy and Astrophysics, 430 (1): 165–186, arXiv:astro-ph/0409579, Bibcode:2005A&A...430..165F, doi:10.1051/0004-6361:20041272, S2CID 17804304.
- ^ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode:2001AJ....122.3466M, doi:10.1086/323920.
- ^ Baumgardt, H.; Dettbarn, C.; Wielen, R. (2000). "Absolute proper motions of open clusters. I. Observational data". Astronomy and Astrophysics Supplement Series. 146 (2): 251. arXiv:astro-ph/0010306. Bibcode:2000A&AS..146..251B. doi:10.1051/aas:2000362. S2CID 7180188.
