Astronomy:Mu1 Cancri
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Cancer[2] |
| Right ascension | 08h 06m 18.396s[3] |
| Declination | +22° 38′ 07.76″[3] |
| Apparent magnitude (V) | +5.99[4] (5.87–6.07)[5] |
| Characteristics | |
| Evolutionary stage | Asymptotic giant branch[6] |
| Spectral type | M3 III[7] |
| B−V color index | +1.66[4] |
| Variable type | Lb[7] |
| Astrometry | |
| Radial velocity (Rv) | +29.61±0.57[8] km/s |
| Proper motion (μ) | RA: −5.831[3] mas/yr Dec.: −9.488[3] mas/yr |
| Parallax (π) | 5.4293 ± 0.1351[3] mas |
| Distance | 600 ± 10 ly (184 ± 5 pc) |
| Absolute magnitude (MV) | −0.79[2] |
| Details | |
| Radius | 56.5+4.8 −5.2[9] R☉ |
| Luminosity | 565±21[9] L☉ |
| Surface gravity (log g) | 0.441[10] cgs |
| Temperature | 3,744+186 −150[9] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
Mu1 Cancri, Latinised from μ1 Cancri, is a variable star in the zodiac constellation of Cancer. Its name is a Bayer designation that is Latinized from μ1 Cancri, and abbreviated Mu1 Cnc or μ1 Cnc. The "1" in the name is because (from Earth) it appears to be close to 10 Cancri, or Mu2 Cancri. It is also known by the variable star designation BL Cancri, or BL Cnc. This star is dimly visible to the naked eye with an apparent visual magnitude that ranges from 5.87 down to 6.07.[5] The position of the star near the ecliptic means it is subject to lunar occultations.[12]
Parallax measurements put this star at about 600 light-years (184 parsecs) from the Sun.[3] At that distance, the visual magnitude is diminished by an extinction factor of 0.28 due to interstellar dust.[13] It is drifting further away with a line of sight velocity of +30 km/s.[8]
The star Mu1 Cancri is an evolved red giant currently on the asymptotic giant branch[6] with a stellar classification of M3 III.[7] The lack of technetium-99 in the spectrum indicates it has not yet gone through third dredge-up.[14] The star has expanded to 57 times the radius of the Sun and it is radiating 565 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 3,774 K.[9]
In 1967, Olin J. Eggen announced his discovery that Mu1 Cancri is a variable star.[15] It was given its variable star designation in 1972.[16] It is a slow irregular variable[7] with thermal pulsation periods of 22.6, 37.8 and 203.7 days.[1]
References
- ↑ 1.0 1.1 "Long-term photometry and periods for 261 nearby pulsating M giants", Monthly Notices of the Royal Astronomical Society 400 (4): 1945–61, 2009, doi:10.1111/j.1365-2966.2009.15588.x, Bibcode: 2009MNRAS.400.1945T.
- ↑ 2.0 2.1 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A XHIP record for this object at VizieR.
- ↑ 3.0 3.1 3.2 3.3 3.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 4.0 4.1 Ducati, J. R. (2002), "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system", CDS/ADC Collection of Electronic Catalogues 2237, Bibcode: 2002yCat.2237....0D.
- ↑ 5.0 5.1 Samus', N. N et al. (2017), "General catalogue of variable stars: Version GCVS 5.1", Astronomy Reports 61 (1): 80, doi:10.1134/S1063772917010085, Bibcode: 2017ARep...61...80S.
- ↑ 6.0 6.1 Eggen, Olin J. (July 1992), "Asymptotic giant branch stars near the sun", Astronomical Journal 104 (1): 275–313, doi:10.1086/116239, Bibcode: 1992AJ....104..275E.
- ↑ 7.0 7.1 7.2 7.3 Lebzelter, T.; Hron, J. (December 2003), "Technetium and the third dredge up in AGB stars. I. Field stars", Astronomy and Astrophysics 411 (3): 5335–42, doi:10.1051/0004-6361:20031458, Bibcode: 2003A&A...411..533L.
- ↑ 8.0 8.1 de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics 546: 14, doi:10.1051/0004-6361/201219219, A61, Bibcode: 2012A&A...546A..61D.
- ↑ 9.0 9.1 9.2 9.3 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. [http://vizier.u-strasbg.fr/viz-bin/VizieR-S?Gaia%20DR2%20 680089968036743936 Gaia DR2 record for this source] at VizieR.
- ↑ Ghosh, Supriyo et al. (April 2019), "Spectral calibration of K-M giants from medium-resolution near-infrared HK-band spectra", Monthly Notices of the Royal Astronomical Society 484 (4): 4619–4634, doi:10.1093/mnras/stz299, Bibcode: 2019MNRAS.484.4619G.
- ↑ "mu.01 Cnc". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=mu.01+Cnc.
- ↑ Schneider, Glenn; Anderson, Chris (April 1993), "Rosemary Hill Observatory Lunar Occultation Summary for 1983-1984", Publications of the Astronomical Society of the Pacific 105: 367, doi:10.1086/133163, Bibcode: 1993PASP..105..367S.
- ↑ 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, doi:10.1051/0004-6361:20041272, Bibcode: 2005A&A...430..165F.
- ↑ Lebzelter, T.; Hron, J. (December 2003), "Technetium and the third dredge up in AGB stars. I. Field stars", Astronomy and Astrophysics 411 (3): 533–542, doi:10.1051/0004-6361:20031458, Bibcode: 2003A&A...411..533L. See CncBL in Table 2.
- ↑ Eggen, O. J. (September 1967), "Narrow and broad band photometry of red stars : I. Northern giants", The Astrophysical Journal Supplement Series 14: 307–358, doi:10.1086/190158, Bibcode: 1967ApJS...14..307E, https://articles.adsabs.harvard.edu/pdf/1967ApJS...14..307E, retrieved 31 December 2024.
- ↑ Kukarkin, B. V. et al. (September 1972), "58th Name-List of Variable Stars", Information Bulletin on Variable Stars 717: 1–36, Bibcode: 1972IBVS..717....1K, https://ibvs.konkoly.hu/pub/ibvs/0701/0717.pdf, retrieved 31 December 2024.
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