Draft:BE Lyncis
Delta Scuti variable star in the constellation Lynx
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BE Lyncis is a white-hued variable star in the northern constellation of Lynx. It has the identifier HD 79889 in the Henry Draper Catalogue; BE Lyn is the variable-star designation. With an apparent magnitude of 8.80, it is too faint to be seen by the naked eye but can be observed via binoculars. It is located at a distance of 821 light-years (252 pc) according to Gaia EDR3 parallax measurements, and is moving away from the Sun at a heliocentric radial velocity of 3.906 km/s.
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| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Lynx |
| Right ascension | 09h 18m 17.18s[1] |
| Declination | +46° 09′ 11.3″[1] |
| Apparent magnitude (V) | 8.8±0.009[2] |
| Characteristics | |
| Spectral type | A3[3]: 36 |
| Variable type | δ Sct |
| Astrometry | |
| Radial velocity (Rv) | 3.9064 km/s |
| Proper motion (μ) | RA: 7.95 mas/yr Dec.: 0.753 mas/yr |
| Parallax (π) | 3.8638±0.0519 mas[1] |
| Distance | 840 ± 10 ly (259 ± 3 pc) |
| Other designations | |
| BE Lyn, BD+46 1490, HD 79889, HIP 45649, SAO 42793, TIC 56914404, TYC 3425-1038-1, 2MASS J09181718+4609112[4] | |
| Database references | |
| SIMBAD | data |
Observational history
The star was included in the Henry Draper Catalogue in 1919 as the 79,889th entry (designation HD 79889) and assigned the spectral type of A3.[3]: 36 HD 79889's variability was first noted during regular UBV observations at the Kvistaberg Observatory in April 1985 and confirmed in October of that year. In 1987, the star was determined to be a very likely high-amplitude dwarf Cepheid with a period of 0.0958697 days (2.30 h), though the possibility it was an older SX Phoenicis variable could not be ruled out.[5] It received the variable-star designation BE Lyn in 1989, classified as a Delta Scuti variable varying from magnitude 8.60 to 9.00.[6]
A gradual decrease in the star's pulsation period was reported in 1991 from the analysis of V-band observations conducted at Xinglong Station between 1988 and 1989.[7] However, follow-up observations carried out at the same observatory in 1992 and between 1993 and 1994 instead revealed a parabolic period increase.[8][9] Around this time, several period measurements yielded slightly discrepant results.[a]