2 Andromedae
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Andromeda |
Right ascension | 23h 02m 36.38176s[1] |
Declination | +42° 45′ 28.0628″[1] |
Apparent magnitude (V) | 5.09[2] (5.26 + 7.43)[3] |
Characteristics | |
2 And A | |
Spectral type | A1V[4] |
U−B color index | +0.10[5] |
B−V color index | +0.08[5] |
2 And B | |
Spectral type | F1V/F4V[3] |
Variable type | δ Sct?[3] |
Astrometry | |
2 And A | |
Radial velocity (Rv) | ±2.4 2.1[6] km/s |
Proper motion (μ) | RA: 56.38[1] mas/yr Dec.: −4.47[1] mas/yr |
Parallax (π) | 7.74 ± 0.51[1] mas |
Distance | 420 ± 30 ly (129 ± 9 pc) |
Absolute magnitude (MV) | ±0.16 −0.39[7] |
2 And B | |
Absolute magnitude (MV) | ±0.16 1.88[7] |
Orbit[3] | |
Period (P) | ±0.509 73.997yr |
Semi-major axis (a) | ±0.011″ 0.225 |
Eccentricity (e) | ±0.056 0.800 |
Inclination (i) | ±46.0 21.7° |
Longitude of the node (Ω) | ±2.0 159.5° |
Periastron epoch (T) | 870.280±0.595 1 |
Argument of periastron (ω) (secondary) | ±3.0 356.4° |
Details | |
2 And A | |
Mass | ±0.1 2.7[7] M☉ |
Luminosity | 130.50[2] L☉ |
Surface gravity (log g) | ±0.12 3.40[7] cgs |
Temperature | ±250 8,950[7] K |
Rotational velocity (v sin i) | 212[8] km/s |
Age | +309 −88 100[9] Myr |
2 And B | |
Mass | ±0.06 1.78[7] M☉ |
Surface gravity (log g) | ±0.16 3.90[7] cgs |
Temperature | ±250 7,720[7] K |
Other designations | |
Database references | |
SIMBAD | 2 And |
2 And A | |
2 And B |
2 Andromedae, abbreviated 2 And, is a binary star[3] system in the northern constellation of Andromeda. 2 Andromedae is the Flamsteed designation. It is a faint star system but visible to the naked eye with a combined apparent visual magnitude of 5.09.[2] Based upon an annual parallax shift of mas, 7.7[1] it is located 420 light years away. The binary nature of the star was discovered by American astronomer Sherburne Wesley Burnham at Lick Observatory in 1889.[11] The pair orbit each other over a period of 74 years with a high eccentricity of 0.8.[3]
The magnitude 5.26[3] primary, designated component A, is an A-type main-sequence star based on a stellar classification of A1V[4] or A2V,[3] although it may have already left the main sequence.[7] It was identified as a candidate Lambda Boötis star, but this was ruled out by Paunzen et al. (2003) as it doesn't match the typical characteristics of these objects.[12] Although 2 And does not display a significant infrared excess, it is a shell star that displays varying absorption features due to circumstellar dust grains. This may indicate it has an orbiting debris disk containing gas that is being viewed edge-on.[13] The star is about 100 million years old and is spinning rapidly with a projected rotational velocity of 212 km/s.[8]
The magnitude 7.43[3] secondary companion, component B, is a suspected variable star and may be a Delta Scuti variable.[3] Alternatively, it may be an ellipsoidal variable with a brown dwarf companion.[7] It is an F-type main-sequence star with a class of F1V/F4.[3]
References
- 1 2 3 4 5 6 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. Vizier catalog entry
- 1 2 3 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015.
- 1 2 3 4 5 6 7 8 9 10 11 Rica Romero, F. M. (2010). "Orbital elements for eight binaries. Study of the nature of wide components. I" (PDF). Revista Mexicana de Astronomía y Astrofísica. 46: 263–277. Bibcode:2010RMxAA..46..263R.
- 1 2 Abt, Helmut A.; Morrell, Nidia I. (1995). "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars". The Astrophysical Journal Supplement Series. 99: 135. Bibcode:1995ApJS...99..135A. doi:10.1086/192182.
- 1 2 Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Bibcode:1986EgUBV........0M.
- ↑ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065.
- 1 2 3 4 5 6 7 8 9 10 Jerzykiewicz, M.; et al. (2015). "The 2003–2004 multisite photometric campaign for the β Cephei and eclipsing star 16 (EN) Lacertae with an appendix on 2 Andromedae, the variable comparison star". Monthly Notices of the Royal Astronomical Society. 454 (1): 724–740. arXiv:1508.05250. Bibcode:2015MNRAS.454..724J. doi:10.1093/mnras/stv1958.
- 1 2 Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy & Astrophysics. 537: A120. arXiv:1201.2052. Bibcode:2012A&A...537A.120Z. doi:10.1051/0004-6361/201117691.
- ↑ Gullikson, Kevin; et al. (August 2016). "The Close Companion Mass-ratio Distribution of Intermediate-mass Stars". The Astronomical Journal. 152 (2): 13. arXiv:1604.06456. Bibcode:2016AJ....152...40G. doi:10.3847/0004-6256/152/2/40. 40.
- ↑ "2 And". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved September 11, 2018.
- ↑ Burnham, S. W. (1894). "Sixteenth Catalogue of New Double Stars Discovered at the Lick Observatory". Publications of Lick Observatory. 2: 197–205. Bibcode:1894PLicO...2..197B.
- ↑ Paunzen, E.; et al. (June 2003). "A study of lambda Bootis type stars in the wavelength region beyond 7000 Å". Astronomy and Astrophysics. 404: 579–591. Bibcode:2003A&A...404..579P. doi:10.1051/0004-6361:20030284.
- ↑ Roberge, Aki; Weinberger, Alycia J. (March 2008). "Debris Disks around Nearby Stars with Circumstellar Gas". The Astrophysical Journal. 676 (1): 509–517. Bibcode:2008ApJ...676..509R. doi:10.1086/527314.