Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Ursa Major |
Right ascension | 09h 36m 53.155s [2] |
Declination | +44° 04′ 00.40″ [2] |
Apparent magnitude (V) | 10.86 to 11.52 [3] |
Characteristics | |
Evolutionary stage | subgiant [4] |
Spectral type | A9 [4] |
Variable type | SX Phe(?) [3] |
Astrometry | |
Radial velocity (Rv) | 150±27 [4] km/s |
Proper motion (μ) |
RA: −15.755
mas/
yr
[2] Dec.: −12.650 mas/ yr [2] |
Parallax (π) | 1.3593 ± 0.0332 mas [2] |
Distance | 2,400 ± 60
ly (740 ± 20 pc) |
Details [4] | |
Mass | 1.805±0.055 M☉ |
Radius | 2.367±0.046 R☉ |
Luminosity | 24.0+2.8 −2.5 L☉ |
Surface gravity (log g) | 3.9543±0.0044 cgs |
Temperature | 8,357+195 −190 K |
Metallicity [Fe/H] | −0.32±0.23 dex |
Age | 1.055±0.095 Gyr |
Other designations | |
Database references | |
SIMBAD | data |
AE Ursae Majoris is a star in the northern circumpolar constellation of Ursa Major, abbreviated AE UMa. It is a variable star that ranges in brightness from a peak apparent visual magnitude of 10.86 down to 11.52. [3] The distance to this star is approximately 2,400 light years based on parallax measurements. [2]
The variability of this star was announced by E. Geyer and associates in 1955. [6] V. P. Tsesevich in 1973 found it to be a dwarf cepheid with a period of 0.086017 days, and he noticed it showed amplitude variations in the light curve. [7] In 1974, B. Szeidl determined a secondary period of 0.066529 days, [8] while P. Broglia and P. Conconi found a beat period of 0.294 days. [9] It belonged to a group of high amplitude, double mode Delta Scuti variables that included SX Phoenicis, [10] and by 1995 it was classified as a SX Phoenicis variable and a possible halo object. However, E. Hintz and associates in 1997 found strong evidence against this classification. [7] [4]
In 2001, the overtone pulsation period of this star was shown to change at the rate of −7.3×10−8 y−1. [11] In addition, possible sudden jumps in the period have been observed, a property it has in common with VZ Cancri. [12] With an estimated mass 1.8 times that of the Sun and an age of a billion years, it is an evolved star that has left the main sequence and is generating energy on a hydrogen-burning shell surrounding a helium core. The metallicity suggests it is a population I Delta Scuti variable. Currently it is crossing the Hertzsprung gap. [4]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Ursa Major |
Right ascension | 09h 36m 53.155s [2] |
Declination | +44° 04′ 00.40″ [2] |
Apparent magnitude (V) | 10.86 to 11.52 [3] |
Characteristics | |
Evolutionary stage | subgiant [4] |
Spectral type | A9 [4] |
Variable type | SX Phe(?) [3] |
Astrometry | |
Radial velocity (Rv) | 150±27 [4] km/s |
Proper motion (μ) |
RA: −15.755
mas/
yr
[2] Dec.: −12.650 mas/ yr [2] |
Parallax (π) | 1.3593 ± 0.0332 mas [2] |
Distance | 2,400 ± 60
ly (740 ± 20 pc) |
Details [4] | |
Mass | 1.805±0.055 M☉ |
Radius | 2.367±0.046 R☉ |
Luminosity | 24.0+2.8 −2.5 L☉ |
Surface gravity (log g) | 3.9543±0.0044 cgs |
Temperature | 8,357+195 −190 K |
Metallicity [Fe/H] | −0.32±0.23 dex |
Age | 1.055±0.095 Gyr |
Other designations | |
Database references | |
SIMBAD | data |
AE Ursae Majoris is a star in the northern circumpolar constellation of Ursa Major, abbreviated AE UMa. It is a variable star that ranges in brightness from a peak apparent visual magnitude of 10.86 down to 11.52. [3] The distance to this star is approximately 2,400 light years based on parallax measurements. [2]
The variability of this star was announced by E. Geyer and associates in 1955. [6] V. P. Tsesevich in 1973 found it to be a dwarf cepheid with a period of 0.086017 days, and he noticed it showed amplitude variations in the light curve. [7] In 1974, B. Szeidl determined a secondary period of 0.066529 days, [8] while P. Broglia and P. Conconi found a beat period of 0.294 days. [9] It belonged to a group of high amplitude, double mode Delta Scuti variables that included SX Phoenicis, [10] and by 1995 it was classified as a SX Phoenicis variable and a possible halo object. However, E. Hintz and associates in 1997 found strong evidence against this classification. [7] [4]
In 2001, the overtone pulsation period of this star was shown to change at the rate of −7.3×10−8 y−1. [11] In addition, possible sudden jumps in the period have been observed, a property it has in common with VZ Cancri. [12] With an estimated mass 1.8 times that of the Sun and an age of a billion years, it is an evolved star that has left the main sequence and is generating energy on a hydrogen-burning shell surrounding a helium core. The metallicity suggests it is a population I Delta Scuti variable. Currently it is crossing the Hertzsprung gap. [4]