TX Camelopardalis

Last updated
TX Camelopardalis
TXCamLightCurve.png
The visual band light curve for TX Camelopardalis, from AAVSO data [1]
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Camelopardalis
Right ascension 05h 00m 50.39s
Declination +56° 10′ 52″
Apparent magnitude  (V)7.8 - 16.9 [2]
Characteristics
Spectral type M8/10III [3]
Variable type Mira [2]
Astrometry
Proper motion (μ)RA: 11.448 [4] mas/yr
Dec.: −21.294 [4] mas/yr
Parallax (π)2.9991±0.3335  mas [4]
Distance approx. 1,100  ly
(approx. 330  pc)
Details
Radius 460, [5] 305-727 [3]   R☉
Luminosity 9,638 [6] -11,360 [5]   L☉
Temperature 2,300 [7] -2,779 [5]   K
Other designations
TX  Cam, Hetzler II 1, IRAS  04566+5606, IRC +60150, RAFGL 664
Database references
SIMBAD data

TX Camelopardalis (abbreviated TX Cam) is a Mira-type variable star in the constellation Camelopardalis. It is a classical long period variable star with pulsational period of 558.7 days. [2] Water masers have been observed around the star. [8]

References

  1. ↑ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
  2. 1 2 3 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: B/gcvs. Bibcode:2009yCat....102025S.
  3. 1 2 Kemball, A. J.; Diamond, P. J. (1997). "Imaging the Magnetic Field in the Atmosphere of TX Camelopardalis". Astrophysical Journal Letters . 481 (2): 111–114. Bibcode:1997ApJ...481L.111K. doi: 10.1086/310664 . S2CID   118664171.
  4. 1 2 3 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.
  5. 1 2 3 De Beck, E.; Decin, L.; De Koter, A.; Justtanont, K.; Verhoelst, T.; Kemper, F.; Menten, K. M. (2010). "Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles. II. CO line survey of evolved stars: derivation of mass-loss rate formulae". Astronomy and Astrophysics . 523: A18. arXiv: 1008.1083 . Bibcode:2010A&A...523A..18D. doi:10.1051/0004-6361/200913771. S2CID   16131273. A18.
  6. ↑ Olivier, Enrico A.; Whitelock, Patricia; Marang, Fred (2001). "Dust-enshrouded asymptotic giant branch stars in the solar neighbourhood". Monthly Notices of the Royal Astronomical Society. 326 (2): 490. arXiv: astro-ph/0103294 . Bibcode:2001MNRAS.326..490O. doi: 10.1046/j.1365-8711.2001.04511.x . S2CID   15509666.
  7. ↑ Lorenz-Martins, S.; Pompeia, L. (2000). "Modelling of oxygen-rich envelopes using corundum and silicate grains". Monthly Notices of the Royal Astronomical Society. 315 (4): 856. Bibcode:2000MNRAS.315..856L. doi: 10.1046/j.1365-8711.2000.03486.x .
  8. ↑ Kemball; Diamond, Philip J.; Gonidakis, Ioannis; Mitra, Modhurita; Yim, Kijeong; Pan, Kuo-Chuan; Chiang, Hsin-Fang (2009). "Multi-epoch imaging polarimetry of the SiO masers in the extended atmosphere of the Mira variable TX Cam". The Astrophysical Journal . 698 (2): 1721–1739. arXiv: 0904.2621 . Bibcode:2009ApJ...698.1721K. doi:10.1088/0004-637X/698/2/1721. S2CID   5465685.


This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.