EQ Pegasi
EQ Pegasi (also known as Gliese 896) is a nearby binary system of two red dwarfs. Both components are flare stars, with spectral types of M4Ve and M6Ve respectively, and a current separation between the components of 5.8 arcseconds. The system is at a distance of 20.4 light-years, and is 950 million years old.[12] The primary star is orbited by one known exoplanet.[4]
  EQ Location of EQ Pegasi in the constellation Pegasus | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Pegasus |
| EQ Pegasi A | |
| Right ascension | 23h 31m 52.173851s[1] |
| Declination | +19° 56′ 14.130398″[1] |
| Apparent magnitude (V) | 10.38 (min)[2] |
| EQ Pegasi B | |
| Right ascension | 23h 31m 52.575338s[3] |
| Declination | +19° 56′ 14.005026″[3] |
| Apparent magnitude (V) | 12.58 (min)[2] |
| Characteristics | |
| EQ Pegasi A | |
| Evolutionary stage | red dwarf |
| Spectral type | M4Ve[2] |
| Variable type | Flare star[2] |
| EQ Pegasi B | |
| Evolutionary stage | red dwarf |
| Spectral type | M6Ve[2] |
| Variable type | Flare star[2] |
| Astrometry | |
| EQ Pegasi A | |
| Radial velocity (Rv) | −0.21±0.82[1] km/s |
| Proper motion (μ) | RA: 578.009±0.035 mas/yr[1] Dec.: −59.769±0.023 mas/yr[1] |
| Parallax (π) | 159.6634 ± 0.0341 mas[1] |
| Distance | 20.428 ± 0.004 ly (6.263 ± 0.001 pc) |
| EQ Pegasi B | |
| Proper motion (μ) | RA: 552.349±0.055 mas/yr[3] Dec.: 20.275±0.036 mas/yr[3] |
| Parallax (π) | 159.9085 ± 0.0513 mas[3] |
| Distance | 20.396 ± 0.007 ly (6.254 ± 0.002 pc) |
| Orbit[4] | |
| Period (P) | 83,664.63 ± 1.98 days (229.0613 ± 0.0054 a) |
| Semi-major axis (a) | 5.05797±0.00043" (31.635±0.033 AU) |
| Eccentricity (e) | 0.108047±0.000053 |
| Inclination (i) | 130.065±0.010° |
| Longitude of the node (Ω) | 255.0919±0.0034° |
| Periastron epoch (T) | 2,401,891.34±1.19 |
| Argument of periastron (ω) (secondary) | 307.1416±0.0045° |
| Details | |
| A | |
| Mass | 0.43599±0.00092[4] M☉ |
| Luminosity | 0.019[5] L☉ |
| Temperature | 3,585[6] K |
| Rotation | 1.061 days[7] |
| B | |
| Mass | 0.16527±0.00025[4] M☉ |
| Luminosity | 0.008[5] L☉ |
| Temperature | 3,309[8] K |
| Rotation | 0.404 days[7] |
| Other designations | |
| EQ Peg A: TYC 1723-23-1, 2MASS J23315208+1956142[10] | |
| EQ Peg B: LFT 1800, LHS 3966, LTT 16920, NLTT 57136, TYC 1723-23-2, 2MASS J23315244+1956138[11] | |
| Database references | |
| SIMBAD | The system |
| A | |
| B | |
Discovery
EQ Pegasi was first noticed to be a binary star by Carl A. Wirtanen who in the course of a systematic survey of the McCormick Observatory photographic plates for M-type dwarfs, detected a companion about two magnitudes fainter at a separation of 3.5 arcseconds.[13]
Both components are also thought to be single-lined spectroscopic binaries, with faint companions that have not been resolved in orbits of a few years.[14]
Planetary system
In 2022, a Jovian planet was discovered in orbit around the system's primary star via radio astrometry. Along with the planet around TVLM 513-46546, this is the first confirmed exoplanet discovered entirely using astrometry.[4]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 2.26±0.57 MJ | 0.64282±0.00068 | 284.39±1.47 | 0.35±0.19 | 69.20±25.61° | — |
In culture
In 1998, it was the basis of a hoax, as a telecommunications company claimed it had discovered "alien" signals originating from the star.[15]
Gallery
An ultraviolet band light curve for a flare on EQ Pegasi B, adapted from Mathioudakis et al. (2006)[17]
References
- Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
- Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- Curiel, Salvador; Ortiz-León, Gisela N.; Mioduszewski, Amy J.; Sanchez-Bermudez, Joel (September 2022). "3D Orbital Architecture of a Dwarf Binary System and Its Planetary Companion". The Astronomical Journal. 164 (3): 93. arXiv:2208.14553. Bibcode:2022AJ....164...93C. doi:10.3847/1538-3881/ac7c66. S2CID 251953478.
- Morales, J. C.; Ribas, I.; Jordi, C. (2008). "The effect of activity on stellar temperatures and radii". Astronomy and Astrophysics. 478 (2): 507. arXiv:0711.3523. Bibcode:2008A&A...478..507M. doi:10.1051/0004-6361:20078324. S2CID 16238033.
- Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- Morin, J.; Donati, J.-F.; et al. (October 2008). "Large-scale magnetic topologies of mid M dwarfs". Monthly Notices of the Royal Astronomical Society. 390 (2): 567–581. arXiv:0808.1423. Bibcode:2008MNRAS.390..567M. doi:10.1111/j.1365-2966.2008.13809.x. S2CID 11240756.
- Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- "BD+19 5116". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 18 August 2017.
- "BD+19 5116A". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 18 August 2017.
- "BD+19 5116A". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 18 August 2017.
- Crosley, M. K.; Osten, R. A. (2018). "Constraining Stellar Coronal Mass Ejections through Multi-wavelength Analysis of the Active M Dwarf EQ Peg". The Astrophysical Journal. 856 (1). 39. arXiv:1802.03440. Bibcode:2018ApJ...856...39C. doi:10.3847/1538-4357/aaaec2. S2CID 55448675.
- Wirtanen, C. A. (1941). "A New dMe Double Star". Publications of the Astronomical Society of the Pacific. 53 (316): 340. Bibcode:1941PASP...53..340W. doi:10.1086/125371.
- Tokovinin, A. "Multiple Star Catalog". Retrieved 2019-08-12.
- "BBC News | Sci/Tech | Alien hoax dismays scientists". news.bbc.co.uk. Retrieved 2018-09-25.
- Norton, A. J.; Wheatley, P. J.; West, R. G.; Haswell, C. A.; Street, R. A.; Collier Cameron, A.; Christian, D. J.; Clarkson, W. I.; Enoch, B.; Gallaway, M.; Hellier, C.; Horne, K.; Irwin, J.; Kane, S. R.; Lister, T. A.; Nicholas, J. P.; Parley, N.; Pollacco, D.; Ryans, R.; Skillen, I.; WilsonD. M. (May 2007). "New periodic variable stars coincident with ROSAT sources discovered using SuperWASP". Astronomy and Astrophysics. 467 (2): 785–905. arXiv:astro-ph/0702631. Bibcode:2007A&A...467..785N. doi:10.1051/0004-6361:20077084. S2CID 16358048. Retrieved 11 February 2022.
- Mathioudakis, M.; Bloomfield, D. S.; Jess, D. B.; Dhillon, V. S.; Marsh, T. R. (September 2006). "The periodic variations of a white-light flare observed with ULTRACAM". Astronomy and Astrophysics. 456 (1): 323–327. arXiv:astro-ph/0605196. Bibcode:2006A&A...456..323M. doi:10.1051/0004-6361:20054752. S2CID 8572363. Retrieved 12 February 2022.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.