AE Ursae Majoris

AE Ursae Majoris

A light curve for AE Ursae Majoris, plotted from TESS data[1]
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]
Distance2,400 ± 60 ly
(740 ± 20 pc)
Details[4]
Mass1.805±0.055 M☉
Radius2.367±0.046 R☉
Luminosity24.0+2.8
−2.5 L☉
Surface gravity (log g)3.9543±0.0044 cgs
Temperature8,357+195
−190 K
Metallicity [Fe/H]−0.32±0.23 dex
Age1.055±0.095 Gyr
Other designations
AE UMa, HIP 47181, 2MASS J09365316+4404004[5]
Database references
SIMBADdata

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]

  1. ^ Cite error: The named reference MAST was invoked but never defined (see the help page).
  2. ^ a b c d e Cite error: The named reference GaiaEDR3 was invoked but never defined (see the help page).
  3. ^ a b c Cite error: The named reference Samus_et_al_2017 was invoked but never defined (see the help page).
  4. ^ a b c d e f Cite error: The named reference Niu_et_al_2017 was invoked but never defined (see the help page).
  5. ^ Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  6. ^ Cite error: The named reference Geyer_et_al_1955 was invoked but never defined (see the help page).
  7. ^ a b Cite error: The named reference Hintz_et_al_1997 was invoked but never defined (see the help page).
  8. ^ Cite error: The named reference Szeidl_1974 was invoked but never defined (see the help page).
  9. ^ Cite error: The named reference Broglia_Conconi_1974 was invoked but never defined (see the help page).
  10. ^ Cite error: The named reference Andreasen_1983 was invoked but never defined (see the help page).
  11. ^ Cite error: The named reference Szeidl_2001 was invoked but never defined (see the help page).
  12. ^ Cite error: The named reference Coates_Landes_2008 was invoked but never defined (see the help page).