Astronomy:WOH G17
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Mensa |
| Right ascension | 04h 39m 23.670s[1] |
| Declination | −73° 11′ 02.68″[1] |
| Apparent magnitude (V) | 13.8[2] |
| Characteristics | |
| Evolutionary stage | RSG or AGB[3] |
| Spectral type | M[4] |
| Apparent magnitude (K) | 5.52 |
| Apparent magnitude (G) | 11.15 |
| Apparent magnitude (H) | 5.59 |
| Apparent magnitude (J) | 6.92 |
| Variable type | LPV (Mira or SR)[1] |
| Astrometry | |
| Radial velocity (Rv) | 101.213[5] km/s |
| Proper motion (μ) | RA: 2.293[1] mas/yr Dec.: 7.034[1] mas/yr |
| Parallax (π) | 0.1773 ± 0.0435[1] mas |
| Distance | approx. 18,000 ly (approx. 6,000 pc) |
| Details | |
| Luminosity | 932,967[6] L☉ |
| Surface gravity (log g) | +0.5[6] cgs |
| Temperature | 3,300[6] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
WOH G17 is a possible red supergiant (RSG) located in the Large Magellanic Cloud (LMC) or a Mira variable asymptotic giant branch (AGB) star[3] in the constellation of Mensa. The star is often considered to be a foreground object; much closer than the LMC, probably in the Milky Way, and therefore is potentially much smaller and less luminous.[6]
As a red supergiant, it would be one of the largest known stars, with a luminosity of 933,000 L☉ and temperature of 3,300 K implying a radius of about 2,955 solar radii (2.056×109 km; 13.74 astronomical unit|au),[6] which is somewhat on par with the largest red supergiants known. This would correspond to a volume 25.8 billion times bigger than the Sun. If placed at the center of the Solar system its photosphere would engulf the orbit of Saturn and reach to about 3/4 the distance to Uranus’s orbit.
See also
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 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.
- ↑ Henden, Arne A.; Levine, Stephen; Terrell, Dirk; Welch, Douglas L. (2015). "APASS - the Latest Data Release". American Astronomical Society Meeting Abstracts #225 225: 336.16. Bibcode: 2015AAS...22533616H.
- ↑ 3.0 3.1 Kastner, Joel H.; Thorndike, Stephen L.; Romanczyk, Paul A.; Buchanan, Catherine L.; Hrivnak, Bruce J.; Sahai, Raghvendra; Egan, Michael (2008). "The Large Magellanic Cloud's Top 250: Classification of the Most Luminous Compact 8 μm Sources in the Large Magellanic Cloud". The Astronomical Journal 136 (3): 1221–1241. doi:10.1088/0004-6256/136/3/1221. Bibcode: 2008AJ....136.1221K.
- ↑ Westerlund, B. E.; Olander, N.; Hedin, B. (1981). "Supergiant and giant M type stars in the Large Magellanic Cloud". Astronomy and Astrophysics Supplement Series 43: 267. Bibcode: 1981A&AS...43..267W.
- ↑ Kordopatis, G.; Gilmore, G.; Steinmetz, M.; Boeche, C.; Seabroke, G. M.; Siebert, A.; Zwitter, T.; Binney, J. et al. (2013). "The Radial Velocity Experiment (RAVE): Fourth Data Release". The Astronomical Journal 146 (5): 134. doi:10.1088/0004-6256/146/5/134. Bibcode: 2013AJ....146..134K.
- ↑ 6.0 6.1 6.2 6.3 6.4 Groenewegen, Martin A. T.; Sloan, Greg C. (2018). "Luminosities and mass-loss rates of Local Group AGB stars and Red Supergiants". Astronomy & Astrophysics 609: A114. doi:10.1051/0004-6361/201731089. ISSN 0004-6361. Bibcode: 2018A&A...609A.114G.
 |
