Astronomy:AE Ursae Majoris

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Short description: Variable star in the constellation Ursa Major
AE Ursae Majoris
AEUMaLightCurve.png
A light curve for AE Ursae Majoris, plotted from TESS data[1]
Observation data
Equinox J2000.0]] (ICRS)
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[2] mas/yr
Dec.: −12.650[2] mas/yr
Parallax (π)1.3593 ± 0.0332[2] mas
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]

References

  1. ↑ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html, retrieved 22 September 2022. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G.  Gaia EDR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 3.2 Samus, N. N. et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1 61 (1): 80–88, doi:10.1134/S1063772917010085, Bibcode: 2017ARep...61...80S. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 Niu, Jia-Shu et al. (May 2017), "AE Ursae Majoris - a δ Scuti star in the Hertzsprung Gap", Monthly Notices of the Royal Astronomical Society 467 (3): 3122–3139, doi:10.1093/mnras/stx125, Bibcode: 2017MNRAS.467.3122N. 
  5. ↑ "AE UMa". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=AE+UMa. 
  6. ↑ Geyer, E. et al. (1955), "Kleine Veroeffentl", Remeis Observatory Bamberg: p. 9. 
  7. ↑ 7.0 7.1 Hintz, E. et al. (October 1997), "Time-Series Ensemble Photometry of SX Phoenicis Stars. II. AE Ursae Majoris", Publications of the Astronomical Society of the Pacific 109: 1073–1076, doi:10.1086/133977, Bibcode: 1997PASP..109.1073H. 
  8. ↑ Szeidl, B. (June 1974), "The Secondary Period of AE UMa", Information Bulletin on Variable Stars 903: 1, Bibcode: 1974IBVS..903....1S. 
  9. ↑ Broglia, P.; Conconi, P. (September 1974), "On the Beat Period of AE UMa", Information Bulletin on Variable Stars 923: 1, Bibcode: 1974IBVS..923....1B. 
  10. ↑ Andreasen, G. K. (May 1983), "Delta Scuti variables. II. Comparisons of theoretical evolution sequences with observational data.", Astronomy and Astrophysics 121: 250–258, Bibcode: 1983A&A...121..250A. 
  11. ↑ Szeidl, B. (July 2001), "The small period change of the Delta Scuti star AE UMa", Communications in Asteroseismology 140: 56, Bibcode: 2001CoAst.140...56S. 
  12. ↑ Coates, D. W.; Landes, H. (April 2008), "The beat-curve approach applied to AE UMa", Communications in Asteroseismology 153: 8–16, doi:10.1553/cia_153s8, Bibcode: 2008CoAst.153....8C. 

Further reading

  • Pena, J. H. et al. (November 2016), "Pulsational stability of the SX Phe star AE UMa", Information Bulletin on Variable Stars 6186 (6186): 1, doi:10.22444/IBVS.6186, Bibcode: 2016IBVS.6186....1P. 
  • Zhou, A. -Y. (July 2001), "Period and amplitude variations in the high-amplitude delta Scuti star AE Ursae Majoris", Astronomy and Astrophysics 374: 235–242, doi:10.1051/0004-6361:20010722, Bibcode: 2001A&A...374..235Z. 
  • Pejcha, O. et al. (May 2001), "Times of Maximum Light for AE Ursae Majoris", Information Bulletin on Variable Stars 5080: 1, Bibcode: 2001IBVS.5080....1P. 
  • Pócs, M. D.; Szeidl, B. (March 2001), "Stability of pulsation of the double-mode high-amplitude δ Scuti star AE Ursae Majoris", Astronomy and Astrophysics 368 (3): 880–887, doi:10.1051/0004-6361:20010043, Bibcode: 2001A&A...368..880P. 
  • Szeidl, B.; Viraghalmy, G. (September 2000), "UBVRI Photometry of AE Ursae Maioris at Konkoly Observatory (1974-1998)", Communications of the Konkoly Observatory 98: 303, Bibcode: 2000CoKon..98..303S. 
  • Broglia, P.; Conconi, P. (November 1975), "Beat phenomena in the dwarf cepheid AE UMa", Astronomy and Astrophysics Supplement Series 22: 243–261, Bibcode: 1975A&AS...22..243B. 




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