Astronomy:HU Delphini
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Short description: Star in the constellation Delphinus
250px A visual band light curve for HU Delphini, plotted from ASAS-SN data.[1] The main plot shows the long-term variability, and the inset plot shows the periodic variability. | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Delphinus |
| Right ascension | 20h 29m 48.344s[2] |
| Declination | +09° 41′ 20.25″[2] |
| Apparent magnitude (V) | 13.07[3] |
| Characteristics | |
| Spectral type | M4.5V[4] |
| U−B color index | +1.29[5] |
| B−V color index | +1.64[5] |
| Variable type | Flare star[6] |
| Astrometry | |
| Radial velocity (Rv) | -34.24 ± 0.07[3] km/s |
| Proper motion (μ) | RA: 673.1[3] mas/yr Dec.: 122.0[3] mas/yr |
| Parallax (π) | 113.4 ± 0.2[3] mas |
| Distance | 28.76 ± 0.05 ly (8.82 ± 0.02 pc) |
| Absolute magnitude (MV) | 13.46 / 16.73[3] |
| Orbit[7] | |
| Period (P) | 1.47080±0.00031 yr |
| Semi-major axis (a) | 0.0971±0.0006″ |
| Eccentricity (e) | 0.6232±0.0059 |
| Inclination (i) | 162±3° |
| Longitude of the node (Ω) | 282±2° |
| Periastron epoch (T) | 2019.1567±0.0033 |
| Argument of periastron (ω) (secondary) | 9.6±2.3° |
| Semi-amplitude (K1) (primary) | 5.66±0.61 km/s |
| Semi-amplitude (K2) (secondary) | 11.15±0.63 km/s |
| Details[3] | |
| HU Del A | |
| Mass | 0.237 ± 0.004 M☉ |
| Metallicity [Fe/H] | 0.07 dex |
| Rotation | 0.3085±0.0005[8] days |
| Rotational velocity (v sin i) | 35.1±0.2[8] km/s |
| HU Del B | |
| Mass | 0.114 ± 0.002 M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
| ARICNS | A |
| B | |
HU Delphini, also known as Gliese 791.2, is a star system in the constellation of Delphinus. Its apparent magnitude is 13.07.[3] With a trigonometric parallax of 113.4 ± 0.2 mas,[3] it is about 28.76 light-years (8.82 parsecs) away from the Solar System.
HU Delphini is a binary star with a well-defined period of 1.47080 years and a somewhat high eccentricity of 0.6232. The orbit has been determined from imaging and radial velocity.[7]
Both stars in the system are red dwarfs. The primary component of the system is only 23.7% as massive as the Sun,[3] so it is fully convective.[4] As a result, there are frequent starspots on its surface, especially near poles.[8] While the normal surface temperature of the primary is 3000 K, the starspots themselves are slightly cooler, at about 2700 K. It is also a flare star,[4] the first flare been detected in August 2000.[9] The secondary star has a mass of 11.4% that of the Sun.[3]
See also
References
- ↑ "ASASSN-V J202948.39+094121.2 / HU Del". All Sky Automated Survey for SuperNovae. https://asas-sn.osu.edu/variables/ef24d96a-fdaa-5337-bdc0-7ed249970f91.
- ↑ 2.0 2.1 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E. et al. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues 2246: II/246. Bibcode: 2003yCat.2246....0C. http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II/246.
- ↑ 3.00 3.01 3.02 3.03 3.04 3.05 3.06 3.07 3.08 3.09 3.10 Benedict, G. F.; Henry, T. J.; Franz, O. G.; McArthur, B. E.; Wasserman, L. H.; Jao, Wei-Chun; Cargile, P. A.; Dieterich, S. B. et al. (2016). "The Solar Neighborhood. XXXVII. The Mass–Luminosity Relation for Main-Sequence M Dwarfs". The Astronomical Journal 152 (5): 141. doi:10.3847/0004-6256/152/5/141. Bibcode: 2016AJ....152..141B.
- ↑ 4.0 4.1 4.2 Barnes, J. R.; Jeffers, S. V.; Jones, H. R. A.; Pavlenko, Ya. V.; Jenkins, J. S.; Haswell, C. A.; Lohr, M. E. (2015). "Starspot Distributions on Fully Convective M Dwarfs: Implications for Radial Velocity Planet Searches". The Astrophysical Journal 812 (1): 42. doi:10.1088/0004-637X/812/1/42. Bibcode: 2015ApJ...812...42B.
- ↑ 5.0 5.1 Nicolet, B. (1978). "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System". Astronomy and Astrophysics Supplement Series 34: 1–49. Bibcode: 1978A&AS...34....1N.
- ↑ 6.0 6.1 "GJ 791.2". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=GJ+791.2.
- ↑ 7.0 7.1 Vrijmoet, Eliot Halley; Tokovinin, Andrei; Henry, Todd J.; Winters, Jennifer G.; Jao, Wei-Chun; Horch, Elliott (March 2026). "The Solar Neighborhood LIV: 54 Orbits of M Dwarf Multiples within 30 pc with Speckle Interferometry at SOAR" (in en). The Astronomical Journal 171 (3): 186. doi:10.3847/1538-3881/ae3b40. ISSN 0004-6256. Bibcode: 2026AJ....171..186V.
- ↑ 8.0 8.1 8.2 Barnes, J. R.; Jeffers, S. V.; Haswell, C. A.; Jones, H. R. A.; Shulyak, D.; Pavlenko, Ya. V.; Jenkins, J. S. (2017), "Surprisingly different star-spot distributions on the near equal-mass equal-rotation-rate stars in the M dwarf binary GJ 65 AB", Monthly Notices of the Royal Astronomical Society 471 (1): 811–823, doi:10.1093/mnras/stx1482, Bibcode: 2017MNRAS.471..811B
- ↑ Natsvlishvili R. Sh., Karapetian A. A. A possible flare of a red dwarf HU Del
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