NGC 4349-127 is a probable red giant star approximately 6,100 light-years away in the constellation of Crux. It is a member of the open cluster NGC 4349 (hence the name NGC 4349-127).[4] Its mass is estimated at 3.9 times Solar, and its age is about 200 million years.[4]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Crux |
| Right ascension | 12h 24m 35.47095s[1] |
| Declination | −61° 49′ 11.8614″[1] |
| Apparent magnitude (V) | 10.82[2] |
| Astrometry | |
| Radial velocity (Rv) | −11.20±0.21[1] km/s |
| Proper motion (μ) | RA: −7.848(12) mas/yr[1] Dec.: −0.207(13) 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[citation needed] |
| Details[3] | |
| Mass | 3.01±0.24 M☉ |
| Radius | 37.97±2.56 R☉ |
| Luminosity | 575.4 L☉ |
| Surface gravity (log g) | 1.78±0.05 cgs |
| Temperature | 4417±12 K |
| Metallicity [Fe/H] | −0.17±0.02 dex |
| Rotational velocity (v sin i) | 4.81 km/s |
| Age | 0.32 Gyr |
| 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.[4]
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.[5] Another study by the same team in 2023 also confirms the stellar origin of the signal.[3] A 2024 study also found the radial velocity signal to be caused by non-radial oscillations.[6]
See also
editReferences
edit- ^ a b c d e 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.
- ^ a b "NGC 4349 127". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 November 2023.
- ^ a b Delgado Mena, E.; Gomes da Silva, J.; et al. (November 2023). "Planets around evolved intermediate-mass stars. III. Planet candidates and long-term activity signals in six open clusters". Astronomy & Astrophysics. 679: A94. arXiv:2309.13589. Bibcode:2023A&A...679A..94D. doi:10.1051/0004-6361/202346890.
- ^ a b c 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. S2CID 119483881.
- ^ Spaeth, Dane; Reffert, Sabine; Hunt, Emily L.; Kaminski, Adrian; Quirrenbach, Andreas (2024-07-26). "Non-radial oscillations mimicking a brown dwarf orbiting the cluster giant NGC 4349 No. 127". Astronomy & Astrophysics. arXiv:2407.21583. doi:10.1051/0004-6361/202450163. ISSN 0004-6361.
External links
edit- "Notes for star NGC 4349 No 127". Extrasolar Planets Encyclopaedia. Archived from the original on 2012-09-29. Retrieved 2007-12-21.
- SIMBAD NGC 4349 127b
 | This giant-star-related article is a stub. You can help Wikipedia by expanding it. |