AE Ursae Majoris
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Star AE Ursae Majoris |
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| AladinLite | |||||||||
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Observation dates equinox : J2000.0 , epoch : J2000.0 |
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| Constellation | Big Bear | ||||||||
| Right ascension | 09 h 36 m 53.16 s | ||||||||
| declination | + 44 ° 04 ′ 0.4 ″ | ||||||||
| Apparent brightness | 11.35 (10.86 to 11.52) mag | ||||||||
| Typing | |||||||||
| B − V color index | (0.19) | ||||||||
| Spectral class | A9 | ||||||||
| Variable star type | suspects SXPHE | ||||||||
| Astrometry | |||||||||
| Radial velocity | (−15.7) km / s | ||||||||
| parallax | 1.28 ± 0.07 mas | ||||||||
| distance | (2550 ± 150) ly (800) pc |
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| Proper movement | |||||||||
| Rec. Share: | (−15.91 ± 0.10) mas / a | ||||||||
| Dec. portion: | (−12.75 ± 0.10) mas / a | ||||||||
| Physical Properties | |||||||||
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Other names and catalog entries |
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AE Ursae Majoris is a pulsation-variable star in the constellation Great Bear . The star belongs to the SX Phoenix stars , a subclass of the Delta Scuti stars .
properties
AE UMa is a star of the spectral class A9, and thus has a surface temperature of 7500 to 9750 Kelvin, thus a hot star. In the Hertzsprung-Russell diagram , the star is located above the main sequence in the so-called instability strip (also known as the Hertzsprung gap ).
The SX Phoenix stars are characterized by a short period of 0.7 to a maximum of 2 hours.
Pulsation variability
AE UMa is a multiperiodic pulsation-variable star. So it happens that two periods overlap. The duration of the primary period and thus the maximum period that can be observed is 0.0860171755 days (2.0644093 hours). The second period was determined to be 0.06652840 days, but is not dominant.
The multi-period also affects the brightness maximum and minimum of the light curve. The maximum brightness in the V-band is 10.86 magnitudes (apparent brightness). The minimum is 11.52 magnitudes in the V-band. However, the multi-period also affects the maximum and minimum brightness.
Pulsation class
Originally the star AE UMa was assigned to the pulsation class of the SX Phoenix stars (according to SX Phoenicis ), a subclass of the Delta Scuti stars
However, in a "Publication of the Astronomical Society of the Pacific" it was discussed that AE UMa is not a low-metal star (−0.1 to −0.4 [Fe / H]) due to its comparatively high metallicity .
This value contradicts the definition of the SX-Phoenix stars, since they must have a low metallicity . Due to this fact and the decreasing period, the publication proposes a classification of the star AE UMa in the group of population I dwarf Cepheids (Delta Scuti stars). This erroneous classification as a SX Phoenix star is explained by the properties of the light curve.
Individual evidence
- ↑ a b c d e f g AE UMa. In: SIMBAD . Center de Données astronomiques de Strasbourg , accessed September 14, 2018 .
- ↑ a b c Christopher Watson: VSX: Detail for AE UMa. Retrieved September 14, 2018 .
- ^ AE Ursae Majoris | aavso.org. Retrieved June 6, 2018 .
- ↑ 1997PASP..109.1073H Page 1073. Retrieved June 6, 2018 .