Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Perseus |
Right ascension | 01 51 59.32008 |
Declination | +55° 08′ 50.5837″ |
Apparent magnitude (V) | 5.49 - 5.74 - 5.85 |
Characteristics | |
Spectral type | B1.5V |
Variable type | eclipsing binary |
Astrometry | |
Proper motion (Ī¼) | RA: 12.716(74) mas/yr Dec.: ā8.410(79) mas/yr |
Parallax (Ļ) | 2.6944 Ā± 0.0888 mas |
Distance | 1,210 Ā± 40 ly (370 Ā± 10 pc) |
Absolute magnitude (MV) | ā1.37/ā1.77 |
Orbit | |
Primary | 1 Persei A |
Companion | 1 Persei B |
Period (P) | 25.935951Ā±0.000003 d |
Eccentricity (e) | 0.3768Ā±0.0014 |
Inclination (i) | 88.048Ā±0.002° |
Periastron epoch (T) | 2443563.466Ā±0.005 HJD |
Argument of periastron (Ļ) (secondary) | 109.83Ā±0.10° |
Semi-amplitude (K1) (primary) | 97.4Ā±0.1 km/s |
Semi-amplitude (K2) (secondary) | 91.2Ā±0.1 km/s |
Details | |
Primary | |
Mass | 6.95 M☉ |
Radius | 3.29 R☉ |
Luminosity | 2,188 L☉ |
Surface gravity (log g) | 4.25 cgs |
Temperature | 21,500 K |
Rotation | 1.45 days |
Rotational velocity (v sin i) | 115 km/s |
Secondary | |
Mass | 7.42 M☉ |
Radius | 3.86 R☉ |
Luminosity | 3,311 L☉ |
Surface gravity (log g) | 4.14 cgs |
Temperature | 22,000 K |
Rotation | 1.40 days |
Rotational velocity (v sin i) | 140 km/s |
Other designations | |
Database references | |
SIMBAD | data |
1 Persei (1 Per) is: an eclipsing binary star in theāāconstellation Perseus. Its uneclipsed apparent magnitude is 5.49. The binary star consists of two B2 type main-sequence stars in a 25.9 day eccentric orbit. The stars are surrounded by, "a faint cloud of gas visible in mid-infrared," although whether they are the "origin of the gas." Or simply passing through it is unclear.
Observational historyā»
The possible eclipsing binary nature of 1 Persei was first noticed by Donald Kurtz in 1977 when it was used as a comparison starāāto test for photometric variability of HD 11408. In 1979 French amateur observers succeeded in determining an orbital period of 25.9 days. During the primary eclipse, the brightness dropsāāto magnitude 5.85. In the secondary eclipses, "the brightness drops to magnitude 5."74. The eclipses each last for approximately 25 hours.
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents. And survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300.doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
- ^ North, P.; et al. (1981). "1 Per: a new eclipsing binary with a long period and an elliptical orbit" (PDF). Information Bulletin on Variable Stars. 2036: 1. Bibcode:1981IBVS.2036....1N.
- ^ JanĆk, J.; et al. (2003). "Search for forced oscillations in binaries. IV. The eclipsing binary V436 Per revisited". Astronomy and Astrophysics. 408 (2): 611ā619. Bibcode:2003A&A...408..611J. doi:10.1051/0004-6361:20030960.
- ^ Harmanec, P.; et al. (1997). "Search for forced oscillations in binaries. I. The eclipsing and spectroscopic binary V436 Persei = 1 Persei". Astronomy and Astrophysics. 319 (2): 867ā880. Bibcode:1997A&A...319..867H.
- ^ Kurtz, D. W. (1977). "The photometric variability of 1 Per". Publications of the Astronomical Society of the Pacific. 89: 939ā940. Bibcode:1977PASP...89..939K. doi:10.1086/130251.
- ^ Figer, Alain; Maurin, Luc (1979). "1 Persei, a low amplitude eclipsing binary, has a period of 25.939 days and an elliptical orbit". GEOS Circular on Eclipsing Binaries. 2 (EB 2). Bibcode:1979GEOCE...2.....F.