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NGC 4349-127 is a probable red giant approximately 6,100 light-years away in the constellation of Crux. As a member of the open cluster NGC 4349 (hence the name NGC 4349-127), it is located about 2000 parsecs (about 6500 light years) from the Sun.[2] Its mass is estimated at 3.9 times Solar, and its age is about 200 million years.[2]
 | This article needs additional citations for verification. (January 2017) |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Crux |
| Right ascension | 12h 24m 35.47095s[1] |
| Declination | −61° 49′ 11.8614″[1] |
| Apparent magnitude (V) | +7.4 |
| Characteristics | |
| Spectral type | M II |
| Astrometry | |
| Radial velocity (Rv) | −11.20±0.21[1] km/s |
| Proper motion (μ) | RA: −7.848±0.012 mas/yr[1] Dec.: −0.207±0.013 mas/yr[1] |
| Parallax (π) | 0.5348 ± 0.0143 mas[1] |
| Distance | 6,100 ± 200 ly (1,870 ± 50 pc) |
| Absolute magnitude (MV) | −4.3 |
| Other designations | |
| Database references | |
| SIMBAD | data |
In 2007, this star was found to have a substellar companion. NGC 4349-127 b is a brown dwarf (based on its mass) with nearly 20 times the mass of Jupiter. Within an eccentricity of about 0.19, its orbit is moderately elliptical, about the same as Mercury in the Solar System. It orbits its host star at a distance of 2.38 AU in a period of 677.8 days. This object was discovered by Christophe Lovis and Michel Mayor of the Geneva Observatory using the radial velocity technique.[2]
However, a 2018 study with the same C. Lovis as an author found that the radial velocity signal corresponding to the proposed substellar companion was most likely caused by stellar activity, and thus the companion does not exist.[3]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (dubious) | ≥19.8 MJ | 2.38 | 677.8 ± 6.2 | 0.19 ± 0.07 | — | — |
See also
References
- Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. arXiv:2208.00211. doi:10.1051/0004-6361/202243940. Gaia DR3 record for this source at VizieR.
- C. Lovis & M. Mayor (2007). "Planets around evolved intermediate-mass stars I. Two substellar companions in the open clusters NGC 2423 and NGC 4349". Astronomy & Astrophysics. 472 (2): 657–664. arXiv:0706.2174. Bibcode:2007A&A...472..657L. doi:10.1051/0004-6361:20077375. S2CID 15173677.
- Delgado Mena, E.; Lovis, C.; et al. (November 2018). "Planets around evolved intermediate-mass stars. II. Are there really planets around IC 4651 No. 9122, NGC 2423 No. 3, and NGC 4349 No. 127?". Astronomy & Astrophysics. 619: A2. arXiv:1807.09608. Bibcode:2018A&A...619A...2D. doi:10.1051/0004-6361/201833152.
External links
- "Notes for star NGC 4349 No 127". The Extrasolar Planets Encyclopaedia. Archived from the original on 2012-09-29. Retrieved 2007-12-21.
- SIMBAD NGC 4349 127b
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На других языках
- [en] NGC 4349-127
[ru] NGC 4349-127
NGC 4349-127 — красный гигант спектрального класса M III в созвездии Южного Креста на расстоянии примерно 6270 световых лет от Солнечной системы. Звезда относится к рассеянному звёздному скоплению NGC 4349, которое расположено примерно в 6500 световых годах (2000 пк) от Солнца. Масса звезды составляет порядка 4 солнечных массы, а возраст — 200 млн лет[6]. В 2007 году на орбите звезды был обнаружен субзвёздный компаньон[7], вероятно, коричневый карлик.Другой контент может иметь иную лицензию. Перед использованием материалов сайта WikiSort.org внимательно изучите правила лицензирования конкретных элементов наполнения сайта.
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