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HR 7578 (also known as V4200 Sagittarii) is a binary star in the constellation of Sagittarius. Their combined apparent magnitude is 6.18.[3] Parallax measurements by the Gaia spacecraft put the system at 46.01 light-years (14.107 parsecs) away, making this a nearby system.[2]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Sagittarius |
| Right ascension | 19h 54m 17.17.7453s[2] |
| Declination | −23° 56′ 27.8630″[2] |
| Apparent magnitude (V) | 6.18[3] |
| Characteristics | |
| Spectral type | K3 V + K3 V[4] |
| U−B color index | +0.915[5] |
| B−V color index | +1.045[5] |
| Variable type | BY Dra[3] |
| Astrometry | |
| Radial velocity (Rv) | −5.1 ± 0.2[6] km/s |
| Proper motion (μ) | RA: −124.476±0.067[2] mas/yr Dec.: −410.440±0.043[2] mas/yr |
| Parallax (π) | 70.8873 ± 0.0399 mas[2] |
| Distance | 46.01 ± 0.03 ly (14.107 ± 0.008 pc) |
| Orbit[7] | |
| Primary | HR 7578A |
| Companion | HR 7578B |
| Period (P) | 46.816103±0.000057 d |
| Eccentricity (e) | 0.68640±0.00028 |
| Periastron epoch (T) | 2455441.0477±0.0030 HJD |
| Argument of periastron (ω) (secondary) | 241.168±0.046° |
| Semi-amplitude (K1) (primary) | 47.84±0.033 km/s |
| Semi-amplitude (K2) (secondary) | 48.686±0.031 km/s |
| Details | |
| Rotational velocity (v sin i) | 2.0[4] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
| ARICNS | data |
The two stars of HR 7578 are fairly old, older than the Pleiades but possibly younger than the Hyades.[6] The stars are between 5×108 and 2×109 years old.[6] Both are K-type main-sequence stars.[4] Both stars have a minimum mass of 0.85 ± 0.03 M☉, and are unusually metal-rich, showing high amounts of cyanide and sodium in their spectra.[6]
HR 7578 is a BY Draconis variable. This is a class of variable star whose variability comes from starspots on the stars' surfaces. HR 7578 also has a common proper motion companion, 2MASS J19542064−2356398. It is a red dwarf that is at least 580 astronomical units from the central star system.[3]
References
- "Light Curve". Hipparcos ESA. ESA. Retrieved 17 February 2022.
- 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.
- Chini, R.; Fuhrmann, K.; Barr, A.; Pozo, F.; Westhues, C.; Hodapp, K. (2014). "New visual companions of solar-type stars within 25 pc". Monthly Notices of the Royal Astronomical Society. 437 (1): 879–886. arXiv:1310.2684. Bibcode:2014MNRAS.437..879C. doi:10.1093/mnras/stt1953. S2CID 118717758.
- Pasquini, L.; Cortés, C.; Lombardi, M.; Monaco, L.; Leão, I. C.; Delabre, B. (2015). "Tachoastrometry: Astrometry with radial velocities". Astronomy & Astrophysics. 574: A76. arXiv:1412.7075. Bibcode:2015A&A...574A..76P. doi:10.1051/0004-6361/201424882. S2CID 55059342.
- Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
- Fekel, F. C., Jr.; Beavers, W. I. (1983). "HR 7578 - A K dwarf double-lined spectroscopic binary with peculiar abundances". The Astrophysical Journal. 267: 682. Bibcode:1983ApJ...267..682F. doi:10.1086/160905.
- Fekel, Francis C.; Henry, Gregory W.; Tomkin, Jocelyn (2017). "New Precision Orbits of Bright Double-lined Spectroscopic Binaries. X. HD 96511, HR 7578, and KZ Andromedae". The Astronomical Journal. 154 (3). 120. Bibcode:2017AJ....154..120F. doi:10.3847/1538-3881/aa816e.
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HR 7578 (также известная как V4200 Стрелеца и 242 G. Стрельца[14]) — кратная звёздная система в экваториальном созвездии Стрельца. Звезда имеет видимую звёздную величину +6.18m[2], и, согласно шкале Бортля, видна невооружённым глазом на деревенско-пригородное небе (англ. Rural/suburban transition). Из измерений параллакса, полученных во время миссии Gaia[15], известно, что звезда удалена примерно на 46,01 св. лет (14,107 пк) от Земли. Звезда наблюдается южнее 67° с.ш., т.е. видна практически на всей территории обитаемой Земли, за исключением северных полярных областей. Лучшее время для наблюдения — июль[16].Другой контент может иметь иную лицензию. Перед использованием материалов сайта WikiSort.org внимательно изучите правила лицензирования конкретных элементов наполнения сайта.
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