HN Pegasi
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Pegasus |
| Right ascension | 21h 44m 31.32919s[1] |
| Declination | +14° 46′ 18.9806″[1] |
| Apparent magnitude (V) | 5.940[2] |
| Characteristics | |
| Spectral type | G0 V CH-0.5[3] |
| U−B color index | +0.031[2] |
| B−V color index | +0.588[2] |
| Variable type | BY Dra[4] |
| Astrometry | |
| Radial velocity (Rv) | −16.68±0.09[5] km/s |
| Proper motion (μ) | RA: +229.93[1] mas/yr Dec.: −113.46[1] mas/yr |
| Parallax (π) | 55.91 ± 0.45[1] mas |
| Distance | 58.3 ± 0.5 ly (17.9 ± 0.1 pc) |
| Absolute magnitude (MV) | 4.70[6] |
| Details | |
| HN Peg A | |
| Mass | 1.085±0.091[4] M☉ |
| Radius | 1.002±0.018[4] R☉ |
| Luminosity (bolometric) | 1.090[6] L☉ |
| Surface gravity (log g) | 4.45[7] cgs |
| Temperature | 5,961[7] K |
| Metallicity [Fe/H] | −0.06[7] dex |
| Rotation | 4.84[8] |
| Rotational velocity (v sin i) | 12.81[9] km/s |
| Age | 237±33[4] Myr |
| HN Peg B | |
| Radius | 0.101[10] R☉ |
| Surface gravity (log g) | 4.81[10] cgs |
| Temperature | 1,115[10] K |
| Other designations | |
HN Pegasi is the variable star designation for a young, Sun-like star in the northern constellation of Pegasus. It has an apparent visual magnitude of 5.9,[2] which, according to the Bortle scale, indicates that it is visible to the naked eye from suburban skies. Parallax measurements made by the Hipparcos spacecraft put the star at a distance of around 58 light years.[1]
This is a G-type main sequence star with a stellar classification of G0 V CH-0.5[3] and an estimated age of just 237 million years. It has slightly more mass and a slightly larger radius than the Sun,[4] but a somewhat lower abundance of elements other than hydrogen and helium.[7] It is spinning relatively quickly, with an estimated rotation period of 4.84[8] days.
The surface magnetic field of the star has a complex and variable geometry. It is a BY Draconis variable star with an active chromosphere, which means there is a rotational modulation of its luminosity due to star spots. Much like the Sun, the star spot activity undergoes a periodic cycle of maxima and minima lasting roughly 5.5±0.3 yr.[4] The star shows an anti-solar pattern of rotation, with the rotation rate steadily increasing during each cycle before dropping back to the initial value upon the start of a new cycle.[8]
In 2007, the discovery of a brown dwarf companion was announced. HN Peg B was spotted using the Spitzer Space Telescope at an angular separation of 43.2 arc minutes, showing a methane emission characteristic of T-type dwarfs. The separation corresponds to a projected physical distance of 795 AU,[12] which is uncommonly wide for such brown dwarf companions. The estimated mass of the object is 28 MJ. Based upon its spectrum, HN Peg B has relatively thin cloud decks.[10]
This star displays an emission of infrared excess that suggests there is a circumstellar disk of debris in orbit.[6] HN Pegasus is most likely a thin disk population star.[7] It is a member of the nearby Hercules-Lyra association of stars that share a common motion through space.[4]
References
- 1 2 3 4 5 6 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752
, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357. - 1 2 3 4 Blanco, C.; et al. (1979), "Photoelectric observations of stars with variable H and K emission components. III", Astronomy and Astrophysics Supplement Series, 36: 297–306, Bibcode:1979A&AS...36..297B.
- 1 2 Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637.
- 1 2 3 4 5 6 7 Boro Saikia, S.; et al. (January 2015), "Variable magnetic field geometry of the young sun HN Pegasi (HD 206860)", Astronomy & Astrophysics, 573: 16, arXiv:1410.8307, Bibcode:2015A&A...573A..17B, doi:10.1051/0004-6361/201424096, A17.
- ↑ Nidever, David L.; et al. (August 2002), "Radial Velocities for 889 Late-Type Stars", The Astrophysical Journal Supplement Series, 141 (2): 503–522, arXiv:astro-ph/0112477, Bibcode:2002ApJS..141..503N, doi:10.1086/340570.
- 1 2 3 Ertel, S.; et al. (May 2012), "A peculiar class of debris disks from Herschel/DUNES. A steep fall off in the far infrared", Astronomy & Astrophysics, 541: 14, arXiv:1203.6784, Bibcode:2012A&A...541A.148E, doi:10.1051/0004-6361/201118077, A148.
- 1 2 3 4 5 Ramírez, I.; et al. (February 2013), "Oxygen abundances in nearby FGK stars and the galactic chemical evolution of the local disk and halo", The Astrophysical Journal, 764 (1): 78, arXiv:1301.1582, Bibcode:2013ApJ...764...78R, doi:10.1088/0004-637X/764/1/78.
- 1 2 3 Messina, S.; Guinan, E. F. (October 2003), "Magnetic activity of six young solar analogues II. Surface Differential Rotation from long-term photometry", Astronomy and Astrophysics, 409: 1017−1030, Bibcode:2003A&A...409.1017M, doi:10.1051/0004-6361:20031161.
- ↑ Martínez-Arnáiz, R.; et al. (September 2010), "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter", Astronomy and Astrophysics, 520: A79, arXiv:1002.4391, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725.
- 1 2 3 4 Leggett, S. K.; et al. (August 2008), "HN Peg B: A Test of Models of the L to T Dwarf Transition", The Astrophysical Journal, 682 (2): 1256−1263, arXiv:0804.1386, Bibcode:2008ApJ...682.1256L, doi:10.1086/589146.
- ↑ "V* HN Peg -- Variable of BY Dra type", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2015-12-07.
- ↑ Luhman, K. L.; et al. (January 2007), "Discovery of Two T Dwarf Companions with the Spitzer Space Telescope", The Astrophysical Journal, 654 (1): 570−579, arXiv:astro-ph/0609464, Bibcode:2007ApJ...654..570L, doi:10.1086/509073.