UX Arietis
| Observation data EpochJ2000EquinoxJ2000 | |
|---|---|
| Constellation | Aries |
| Right ascension | 03h26m35.37568s[2] |
| Declination | +28° 42′ 54.2264″[2] |
| Apparent magnitude(V) | 6.35 - 6.71[3] |
| Characteristics | |
| Spectral type | G5IV[4] |
| U−Bcolor index | 0.43[5] |
| B−Vcolor index | 0.90[5] |
| Variable type | RS CVn[6] |
| Astrometry | |
| Radial velocity(Rv) | +26.53[7]km/s |
| Proper motion(μ) | RA:+46.794[2]mas/yr Dec.:−102.876[2]mas/yr |
| Parallax(π) | 19.7836 ± 0.1264mas[2] |
| Distance | 165 ± 1ly (50.5 ± 0.3pc) |
| Absolute magnitude(MV) | 2.91[8] |
| Orbit[9] | |
| Primary | Aa |
| Companion | Ab |
| Period(P) | 6.437888±0.000007d |
| Semi-major axis(a) | 1.750±0.01mas |
| Eccentricity(e) | 0 (fixed) |
| Inclination(i) | 125.0±0.5° |
| Longitude of the node(Ω) | 113.4±0.4° |
| Periastronepoch(T) | 2456238.134 ± 0.002 HJD |
| Argument of periastron(ω) (secondary) | 90 (fixed)° |
| Orbit[10] | |
| Primary | A |
| Companion | B |
| Period(P) | 111.02yr |
| Semi-major axis(a) | 648.0±0.8mas |
| Eccentricity(e) | 0.77±0.01 |
| Inclination(i) | 93.3±0.6° |
| Longitude of the node(Ω) | 58.9±0.5° |
| Periastronepoch(T) | 2451664.9±34.3HJD |
| Argument of periastron(ω) (secondary) | 274.9±0.8° |
| Details[9] | |
| UX Ari Aa | |
| Mass | 1.30±0.06M☉ |
| Radius | 5.6±0.1R☉ |
| Luminosity | 9.3±0.7L☉ |
| Surface gravity(logg) | 3.06±0.04cgs |
| Temperature | 4,560±100K |
| Rotation | 6.44 d[4] |
| UX Ari Ab | |
| Mass | 1.14±0.06M☉ |
| Radius | 1.6±0.2R☉ |
| Luminosity | 2.34±0.28L☉ |
| Surface gravity(logg) | 4.09±0.16cgs |
| Temperature | 5,670±100K |
| UX Ari B | |
| Mass | 0.75M☉ |
| Radius | 0.8±0.1R☉ |
| Luminosity | 0.38±0.08L☉ |
| Surface gravity(logg) | 4.51±0.13cgs |
| Temperature | 4,930±100K |
| Other designations | |
| Database references | |
| SIMBAD | data |
| ARICNS | data |
UX Arietisis atriple starsystem located in the northern zodiacalconstellationofAries.Based uponparallaxmeasurements from theGaiasatellite, it is roughly 165light yearsaway. The primary, component Aa, is avariable starof theRS CVntype. The variability of the star is believed due to a combination of coolstar spotsand warmflares,set against the baseline quiescent temperature of thestellar atmosphere.The variability appears to be cyclical with a period of 8−9 years.[6]The star varies in brightness frommagnitude6.35 to 6.71, meaning it may be intermittently visible to the unaided eye under ideal dark-sky conditions.[3]
A more distant companion, component C, shares acommon proper motionand is at the same distance.[11]It is another cool dwarf star with an estimated spectral class of K2. Any orbit is estimated to require over 100,000 years.[12]
References
[edit]- ^Ulvås, V. Aarum; Henry, G. W. (May 2003)."BV photometry of UX Ari in the period 1987–2002".Astronomy & Astrophysics.402(3): 1033–1041.Bibcode:2003A&A...402.1033A.doi:10.1051/0004-6361:20030304.
- ^abcdeVallenari, A.; et al. (Gaia collaboration) (2023)."GaiaData 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.S2CID244398875. Gaia DR3 record for this sourceatVizieR.
- ^ab"UX Ari".The International Variable Star Index.AAVSO.Retrieved28 October2021.
- ^abStrassmeier, Klaus G. (September 2009)."Starspots".The Astronomy and Astrophysics Review.17(3): 251–308.Bibcode:2009A&ARv..17..251S.doi:10.1007/s00159-009-0020-6.
- ^abGuetter, H. H.; Hewitt, A. V. (June 1984)."Photoelectric UBV photometry for 317 PZT and VZT stars".Publications of the Astronomical Society of the Pacific.96:441–443.Bibcode:1984PASP...96..441G.doi:10.1086/131362.
- ^abAlekseev, I. Yu. (September 2014). "Three-Component Model of Spottedness in the Classical RS CVn System UX Ari".Astrophysics.57(3): 344–351.Bibcode:2014Ap.....57..344A.doi:10.1007/s10511-014-9339-4.S2CID119963417.
- ^Karataș, Yüksel; Bilir, Selçuk; Eker, Zeki; Demircan, Osman; Liebert, James; Hawley, Suzanne L.; Fraser, Oliver J.; Covey, Kevin R.; Lowrance, Patrick; Kirkpatrick, J. Davy; Burgasser, Adam J. (2004)."Kinematics of chromospherically active binaries and evidence of an orbital period decrease in binary evolution".Monthly Notices of the Royal Astronomical Society.349(3): 1069–1092.arXiv:astro-ph/0404219.Bibcode:2004MNRAS.349.1069K.doi:10.1111/j.1365-2966.2004.07588.x.S2CID15290475.
- ^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.eISSN1562-6873.ISSN1063-7737.S2CID119257644.
- ^abHummel, C. A.; et al. (August 2017)."Orbital Elements and Stellar Parameters of the Active Binary UX Arietis".The Astrophysical Journal.844(2): 12.Bibcode:2017ApJ...844..115H.doi:10.3847/1538-4357/aa7b87.hdl:10871/32318.S2CID43383613.115.
- ^Peterson, W. M.; Mutel, R. L.; Lestrade, J. -F.; Güdel, M.; Goss, W. M. (2011). "Radio Astrometry of the Triple Systems Algol and UX Arietis".The Astrophysical Journal.737(2): 104.arXiv:1104.5005.Bibcode:2011ApJ...737..104P.doi:10.1088/0004-637X/737/2/104.S2CID119229905.
- ^Vallenari, A.; et al. (Gaia collaboration) (2023)."GaiaData 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.S2CID244398875. Gaia DR3 record for this sourceatVizieR.
- ^Tokovinin, Andrei (2018-03-01)."The Updated Multiple Star Catalog".The Astrophysical Journal Supplement Series.235(1): 6.arXiv:1712.04750.Bibcode:2018ApJS..235....6T.doi:10.3847/1538-4365/aaa1a5.ISSN0067-0049.S2CID119047709.
Further reading
[edit]- Brinkman, Albert (2000). "High-Resolution Spectrum of UX Ari".Chandra Proposal ID #02200030:434.Bibcode:2000cxo..prop..434B.
- Drake, Stephen (1999). "Acis/hetg Spectroscopy of the Active Binaries Algol & UX Ari".Chandra Proposal ID #01200248:20.Bibcode:1999cxo..prop...20D.
- V. Aarum Ulvås & G. W. Henry (2003)."BV photometry of UX Ari in the period 1987-2002".Astronomy and Astrophysics.
