Astronomy:Gliese 521
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Canes Venatici[1] |
| Right ascension | 13h 39m 24.10228s[2] |
| Declination | +46° 11′ 11.3631″[2] |
| Apparent magnitude (V) | +10.26[3] |
| Characteristics | |
| Evolutionary stage | main sequence[4] |
| Spectral type | M1V[4] |
| Apparent magnitude (J) | 7.05[3] |
| Apparent magnitude (H) | 6.51[3] |
| Apparent magnitude (K) | 6.26[3] |
| Astrometry | |
| Radial velocity (Rv) | −65.72±0.15[2] km/s |
| Proper motion (μ) | RA: −42.332±0.012[2] mas/yr Dec.: 389.167±0.014[2] mas/yr |
| Parallax (π) | 74.7985 ± 0.0153[2] mas |
| Distance | 43.605 ± 0.009 ly (13.369 ± 0.003 pc) |
| Absolute magnitude (MV) | 10.243[5] |
| Details | |
| Mass | 0.506±0.021 M☉[3] 0.47±0.05[6] M☉ |
| Radius | 0.619±0.030 R☉[5] 0.47±0.05[6] R☉ |
| Luminosity | 0.033+0.008 −0.007[6] L☉ |
| Surface gravity (log g) | 4.79±0.04[6] cgs |
| Temperature | 3,493±50[5] K |
| Metallicity [Fe/H] | −0.34 dex[3] −0.09±0.09[6] dex |
| Rotation | 49.5±3.5 d[7] |
| Rotational velocity (v sin i) | 0.85[5] 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.[5] It is predicted to come as close as 15.70 light-years from the Sun in 176,900 years.[9] This star is too faint to be visible to the naked eye, having an apparent visual magnitude of +10.26[3] and an absolute magnitude of 10.24.[5]
The primary is an M-type main-sequence star with a stellar classification of M1V.[4] 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[5] and a rotation period of roughly 49.5 days.[7] The star has a lower metal-content compared to the Sun. It is radiating just 3%[6] of the luminosity of the Sun from its photosphere at an effective temperature of 3,493 K.[5]
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 astronomical unit|AU.[10]
Search for planets
According to Marcy & Benitz (1989)[11] 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.[12]
See also
References
- ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific 99 (617): 695. doi:10.1086/132034. Bibcode: 1987PASP...99..695R Constellation record for this object at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 Jenkins, J. S. et al. (2009). "Rotational Velocities for M Dwarfs". The Astrophysical Journal 704 (2): 975. doi:10.1088/0004-637X/704/2/975. Bibcode: 2009ApJ...704..975J.
- ↑ 4.0 4.1 4.2 Alonso-Floriano, F. J. et al. (May 2015). "CARMENES input catalogue of M dwarfs. I. Low-resolution spectroscopy with CAFOS". Astronomy & Astrophysics 577: 19. doi:10.1051/0004-6361/201525803. A128. Bibcode: 2015A&A...577A.128A.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 5.7 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. doi:10.1111/j.1365-2966.2010.16827.x. Bibcode: 2010MNRAS.407.1657H.
- ↑ 6.0 6.1 6.2 6.3 6.4 6.5 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. doi:10.1051/0004-6361/201629223. A27. Bibcode: 2017A&A...598A..27M.
- ↑ 7.0 7.1 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. doi:10.1051/0004-6361/201732143. A89. Bibcode: 2018A&A...612A..89S.
- ↑ "BD+46 1889". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=BD%2B46+1889.
- ↑ 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. doi:10.1051/0004-6361/201731453. A8. Bibcode: 2018A&A...609A...8B.
- ↑ Jódar, Esther et al. (February 2013). "New companions to nearby low-mass stars". Monthly Notices of the Royal Astronomical Society 429 (1): 859–867. doi:10.1093/mnras/sts382. Bibcode: 2013MNRAS.429..859J.
- ↑ 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. doi:10.1086/167812. Bibcode: 1989ApJ...344..441M.
- ↑ Gonzalez Alvarez, Ester (2018). Planets around low-mass stars and stellar activity effects. Doctoral Thesis (Thesis). Università degli Studi di Palermo. hdl:10447/265375. Retrieved 2021-11-21.
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