Astronomy:V1472 Aquilae
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Aquila |
| Right ascension | 20h 05m 26.54594s[2] |
| Declination | +15° 30′ 01.5408″[2] |
| Apparent magnitude (V) | 6.34[3] (6.36 to 6.60)[4] |
| Characteristics | |
| Spectral type | M2.5III[1] |
| U−B color index | +1.76[3] |
| B−V color index | +1.64[3] |
| Variable type | Candidate eclipsing variable[4] |
| Astrometry | |
| Radial velocity (Rv) | −111.7±0.3[5] km/s |
| Proper motion (μ) | RA: 33.899[2] mas/yr Dec.: 24.023[2] mas/yr |
| Parallax (π) | 4.1626 ± 0.1069[2] mas |
| Distance | 780 ± 20 ly (240 ± 6 pc) |
| Absolute magnitude (MV) | −2.6±1.0[6] |
| Orbit[7] | |
| Period (P) | 198.716±0.038 d |
| Semi-major axis (a) | ≥ 35.39 ± 0.76 Gm (0.2366 ± 0.0051 astronomical unit|AU) |
| Eccentricity (e) | 0.048±0.016 |
| Periastron epoch (T) | 24,443,721.1 |
| Argument of periastron (ω) (secondary) | 99.3±29.7° |
| Semi-amplitude (K1) (primary) | 12.97±0.27 km/s |
| Details | |
| Radius | 104±56[6] R☉ |
| Luminosity | 1,100[6] L☉ |
| Temperature | 3,670[8] K |
| Rotational velocity (v sin i) | 10[8] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
V1472 Aquilae is a triple star system in the equatorial constellation of Aquila. It is a variable star that ranges in brightness from 6.36 down to 6.60.[4] The system is located at a distance of approximately 780 light years from the Sun based on parallax. It is a high-velocity star system with a radial velocity of −112 km/s.[5]
The binary nature of the main component was announced by P. B. Lucke and M. Mayor in 1982, who found it to be a single-lined spectroscopic binary with an orbital period of 198.7 days and an eccentricity of 0.05. At the time of its discovery, it was the shortest known binary period of any class M giant.[7] The primary is an aging red giant with a stellar classification of M2.5III.[1] It has a diameter 104±56 times and luminosity 1,100 times that of the Sun.[6] The star is a fast rotator with a projected rotational velocity of 10 km/s, possibly due to interaction with its companion.[8]
The variability of this star was discovered from Hipparcos data and, in 1997, it was classified as a semiregular variable with a period of 100.3727039 days. However, a plot of the light curve better matches that of an eclipsing binary or ellipsoidal variable. The 198-day orbital period produces a light curve with a primary and secondary minimum which, together with possible variations due to ellipsoidal rotation, produces the observed semiregular 100-day photometric variation.[1] Later observations show that it is less luminous than expected for a pulsating star with its amplitude, being more typical of ellipsoidal variables, and that it has a 200.05-day period with primary and secondary minima.[10]
A co-moving companion some 4.0 magnitudes fainter than the primary lies at an angular separation of 2.7 arcseconds.[1]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Samus, N. N. (1997). "V1472 Aql: a Most Unusual Eclipser?". Information Bulletin on Variable Stars 4501: 1. Bibcode: 1997IBVS.4501....1S.
- ↑ 2.0 2.1 2.2 2.3 2.4 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 Hoffleit, D.; Warren, W. H. (1995). "VizieR Online Data Catalog: Bright Star Catalogue, 5th Revised ed. (Hoffleit+, 1991)". VizieR Online Data Catalog. Bibcode: 1995yCat.5050....0H.
- ↑ 4.0 4.1 4.2 Samus', N. N et al. (2017). "General catalogue of variable stars". Astronomy Reports. GCVS 5.1 61 (1): 80. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S.
- ↑ 5.0 5.1 Famaey, B. et al. (January 12, 2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data: Revisiting the concept of superclusters". Astronomy and Astrophysics 430 (1): 165–186. doi:10.1051/0004-6361:20041272. Bibcode: 2005A&A...430..165F.
- ↑ 6.0 6.1 6.2 6.3 Boffin, H. M. J. et al. (2014). "Roche-lobe filling factor of mass-transferring red giants: the PIONIER view". Astronomy & Astrophysics 564: 13. doi:10.1051/0004-6361/201323194. A1. Bibcode: 2014A&A...564A...1B.
- ↑ 7.0 7.1 Lucke, P. B.; Mayor, M. (January 1982). "Duplicity in the solar neighborhood. II. Spectroscopic orbits for four bright stars HD 21018, HD 30021, HD 158837 and HD 190658". Astronomy and Astrophysics 105: 318–322. Bibcode: 1982A&A...105..318L.
- ↑ 8.0 8.1 8.2 Frankowski, A. et al. (May 2009). "Spectroscopic binaries among Hipparcos M giants. II. Binary frequency". Astronomy and Astrophysics 498 (2): 479–488. doi:10.1051/0004-6361/200810702. Bibcode: 2009A&A...498..479F.
- ↑ "HD 190658". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+190658.
- ↑ Tabur, V.; Bedding, T. R.; Kiss, L. L.; Giles, T.; Derekas, A.; Moon, T. T. (2010). "Period-luminosity relations of pulsating M giants in the solar neighbourhood and the Magellanic Clouds". Monthly Notices of the Royal Astronomical Society 409 (2): 777–788. doi:10.1111/j.1365-2966.2010.17341.x. Bibcode: 2010MNRAS.409..777T.
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