Gliese 521
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Canes Venatici |
| Right ascension | 13h 39m 24.10228s[1] |
| Declination | +46° 11′ 11.3631″[1] |
| Apparent magnitude (V) | +10.26[2] |
| Characteristics | |
| Spectral type | M1V[3] |
| Apparent magnitude (J) | 7.05[2] |
| Apparent magnitude (H) | 6.51[2] |
| Apparent magnitude (K) | 6.26[2] |
| Astrometry | |
| Radial velocity (Rv) | −65.72±0.15[1] km/s |
| Proper motion (μ) | RA: −42.332±0.012 mas/yr[1] Dec.: 389.167±0.014 mas/yr[1] |
| Parallax (π) | 74.7985 ± 0.0153 mas[1] |
| Distance | 43.605 ± 0.009 ly (13.369 ± 0.003 pc) |
| Absolute magnitude (MV) | 10.243[4] |
| Details | |
| Mass | 0.506±0.021 M☉[2] 0.47±0.05[5] M☉ |
| Radius | 0.619±0.030 R☉[4] 0.47±0.05[5] R☉ |
| Luminosity | 0.033+0.008 −0.007[5] L☉ |
| Surface gravity (log g) | 4.79±0.04[5] cgs |
| Temperature | 3,493±50[4] K |
| Metallicity [Fe/H] | −0.34 dex[2] −0.09±0.09[5] dex |
| Rotation | 49.5±3.5 d[6] |
| Rotational velocity (v sin i) | 0.85[4] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
Gliese 521 is a double star in the northern constellation of Canes Venatici. The system is located at a distance of 43.6 light-years from the Sun based on parallax measurements, but is drawing closer with a radial velocity of −65.6 km/s.[4] It is predicted to come as close as 15.70 light-years from the Sun in 176,900 years.[8] This star is too faint to be visible to the naked eye, having an apparent visual magnitude of +10.26[2] and an absolute magnitude of 10.24.[4]
The primary is an M-type main-sequence star with a stellar classification of M1V.[3] It is only about half the size and mass of the Sun. The star is rotating slowly with a projected rotational velocity of 0.85 km/s[4] and a rotation period of roughly 49.5 days.[6] The star has a lower metal-content compared to the Sun. It is radiating just 3%[5] of the luminosity of the Sun from its photosphere at an effective temperature of 3,493 K.[4]
A faint stellar companion was announced by E. Jódar and associates in 2013. The companion has an angular separation of 521 mas along a position angle of 352.1°±1.4° from the primary. This is equivalent to a projected separation of 7.24±0.14 AU.[9]
Search for planets
According to Marcy & Benitz (1989)[10] detected a possible periodicity of 510 days, inferring the possible presence of a massive planetary object with minimum mass of 12 times that of Jupiter in highly eccentric orbit (e=0.6). So far the planet has not been confirmed. A radial velocity study of the star during the period 2013–2017 initially found a promising signal, but this disappeared when additional data was collected and was instead attributed to magnetic activity.[11]
See also
References
- ^ 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 c d e f g Jenkins, J. S.; et al. (2009). "Rotational Velocities for M Dwarfs". The Astrophysical Journal. 704 (2): 975. arXiv:0908.4092. Bibcode:2009ApJ...704..975J. doi:10.1088/0004-637X/704/2/975. S2CID 119203469.
- ^ a b Alonso-Floriano, F. J.; et al. (May 2015). "CARMENES input catalogue of M dwarfs. I. Low-resolution spectroscopy with CAFOS". Astronomy & Astrophysics. 577: 19. arXiv:1502.07580. Bibcode:2015A&A...577A.128A. doi:10.1051/0004-6361/201525803. S2CID 53135130. A128.
- ^ a b c d e f g h Houdebine, E. R. (September 2010). "Observation and modelling of main-sequence star chromospheres - XIV. Rotation of dM1 stars". Monthly Notices of the Royal Astronomical Society. 407 (3): 1657–1673. Bibcode:2010MNRAS.407.1657H. doi:10.1111/j.1365-2966.2010.16827.x.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ a b c d e f Maldonado, J.; et al. (February 2017). "HADES RV Programme with HARPS-N at TNG . III. Flux-flux and activity-rotation relationships of early-M dwarfs". Astronomy & Astrophysics. 598: 19. arXiv:1610.05906. Bibcode:2017A&A...598A..27M. doi:10.1051/0004-6361/201629223. A27.
- ^ a b Suárez Mascareño, A.; et al. (April 2018). "HADES RV programme with HARPS-N at TNG. VII. Rotation and activity of M-dwarfs from time-series high-resolution spectroscopy of chromospheric indicators". Astronomy & Astrophysics. 612: 17. arXiv:1712.07375. Bibcode:2018A&A...612A..89S. doi:10.1051/0004-6361/201732143. A89.
- ^ "BD+46 1889". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-11-21.
- ^ Bailer-Jones, C. A. L. (January 2018). "The completeness-corrected rate of stellar encounters with the Sun from the first Gaia data release". Astronomy & Astrophysics. 609: 16. arXiv:1708.08595. Bibcode:2018A&A...609A...8B. doi:10.1051/0004-6361/201731453. S2CID 119462489. A8.
- ^ Jódar, Esther; et al. (February 2013). "New companions to nearby low-mass stars". Monthly Notices of the Royal Astronomical Society. 429 (1): 859–867. Bibcode:2013MNRAS.429..859J. doi:10.1093/mnras/sts382.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ Marcy, Geoffrey W.; Benitz, Karsten J. (September 1989). "A search for substellar companions to low-mass stars". Astrophysical Journal, Part 1. 344 (1): 441–453. Bibcode:1989ApJ...344..441M. doi:10.1086/167812.
- ^ Gonzalez Alvarez, Ester (2018). Planets around low-mass stars and stellar activity effects. Università degli Studi di Palermo. hdl:10447/265375. Retrieved 2021-11-21.
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