Astronomy:42 Herculis
 42 Herculis in optical light | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Hercules |
| Right ascension | 16h 38m 44.84465s[1] |
| Declination | +48° 55′ 42.0160″[1] |
| Apparent magnitude (V) | 4.86[2] |
| Characteristics | |
| Evolutionary stage | asymptotic giant branch[3] |
| Spectral type | M2.5III[3] |
| B−V color index | 1.562±0.011[2] |
| Astrometry | |
| Radial velocity (Rv) | −55.74±0.33[2] km/s |
| Proper motion (μ) | RA: −47.768[1] mas/yr Dec.: +27.349[1] mas/yr |
| Parallax (π) | 7.2737 ± 0.1764[1] mas |
| Distance | 450 ± 10 ly (137 ± 3 pc) |
| Absolute magnitude (MV) | −0.65[2] |
| Details | |
| Radius | 63.81+5.20 −7.75[1] R☉ |
| Luminosity | 733.6±20.5[1] L☉ |
| Surface gravity (log g) | 1.50[4] cgs |
| Temperature | 3,760.5+251.5 −144.5[1] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
42 Herculis is a single[6] star located around 450[1] light years away from the Sun in the northern constellation of Hercules.[5] It is visible to the naked eye as a faint, red-hued star with an apparent visual magnitude of 4.86.[2] The star is moving closer to the Earth with a heliocentric radial velocity of −56 km/s.[2]
This is an aging red giant star on the asymptotic giant branch with a stellar classification of M2.5III.[3] It has been catalogued as a suspected variable star,[5] although a 1992 photometric survey found the brightness to be constant.[7] Having exhausted the supply of hydrogen at its core, the star has expanded to 64 times the Sun's radius. It is radiating 734 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 3761 K.[1]
There is an unknown source of X-ray and far ultraviolet emission originating from a location offset by more than one arcsecond from the star.[8] This may indicate there is an undetected main sequence companion.[4]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 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. Gaia DR2 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 3.0 3.1 3.2 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.
- ↑ 4.0 4.1 Ortiz, Roberto; Guerrero, Martín A. (September 2016), "Ultraviolet emission from main-sequence companions of AGB stars", Monthly Notices of the Royal Astronomical Society 461 (3): 3036, doi:10.1093/mnras/stw1547, Bibcode: 2016MNRAS.461.3036O.
- ↑ 5.0 5.1 5.2 "42 Her". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=42+Her.
- ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ Percy, J. R.; Shepherd, C. W. (October 1992), "Photometric Survey of Small-Amplitude Red Variables", Information Bulletin on Variable Stars 3792: 1, Bibcode: 1992IBVS.3792....1P.
- ↑ Famaey, B. et al. (2009), "Spectroscopic binaries among Hipparcos M giants. I. Data, orbits, and intrinsic variations", Astronomy and Astrophysics 498 (2): 627–640, doi:10.1051/0004-6361/200810698, Bibcode: 2009A&A...498..627F.
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