Pi1 Ursae Majoris

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For other stars with this name, see Pi Ursae Majoris and Muscida.
Pi1 Ursae Majoris
Diagram showing star positions and boundaries of the Centaurus constellation and its surroundings
Diagram showing star positions and boundaries of the Centaurus constellation and its surroundings

Location of π¹ Ursae Majoris (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Ursa Major
Right ascension 08h 39m 11.70440s[1]
Declination +65° 01′ 15.2667″[1]
Apparent magnitude (V) 5.63
Characteristics
Spectral type G1.5Vb[2]
U−B color index +0.07[3]
B−V color index +0.62[3]
Variable type BY Draconis
Astrometry
Radial velocity (Rv) –13.88 ± 0.47[4] km/s
Proper motion (μ) RA: -27.44 ± 0.31[1] mas/yr
Dec.: +88.13 ± 0.26[1] mas/yr
Parallax (π) 69.66 ± 0.37[1] mas
Distance 46.8 ± 0.2 ly
(14.36 ± 0.08 pc)
Absolute magnitude (MV) 4.86
Details
Mass 0.90[5] M☉
Luminosity 0.97[6] L☉
Surface gravity (log g) 4.48[7] cgs
Temperature 5,884 ± 6.8[8] K
Metallicity [Fe/H] –0.04[7] dex
Rotation 5 days[9]
Rotational velocity (v sin i) 14.27[4] km/s
Age 200[10] Myr
Other designations
π¹ Ursae Majoris, π¹ UMa, Pi1 UMa, 3 Ursae Majoris, BD +65°643, GC 11817, HD 72905, HIP 42438, HR 3391, PPM 16705, SAO 14609.
Database references
SIMBAD data

Pi1 Ursae Majoris (Pi1 UMa, π¹ Ursae Majoris, π¹ UMa) is a yellow G-type main sequence dwarf with a mean apparent magnitude of +5.63. It is approximately 46.8 light years from Earth,[1] and is a relatively young star with an age of about 200 million years.[10] It is classified as a BY Draconis type variable star and its brightness varies by 0.08 magnitudes. In 1986, it became the first solar-type star to have the emission from an X-ray flare observed.[11] Based upon its space velocity components, this star is a member of the Ursa Major moving group of stars that share a common motion through space.[6][9]

An excess of infrared radiation has been detected from this system, which suggests the presence of a debris disk. The best fit to the data indicates that there is a ring of fine debris out to a radius of about 0.4 AU, consisting of 0.25 μm grains of amorphous silicates or crystalline forsterite. There may also be a wider ring of larger (10 μm) grains out to a distance of 16 AU.[12]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Lua error in package.lua at line 80: module 'strict' not found. Note: see VizieR catalogue I/311.
  2. ↑ Lua error in package.lua at line 80: module 'strict' not found.
  3. ↑ 3.0 3.1 Lua error in package.lua at line 80: module 'strict' not found.
  4. ↑ 4.0 4.1 Lua error in package.lua at line 80: module 'strict' not found. Cite error: Invalid <ref> tag; name "aj133_6_2524" defined multiple times with different content
  5. ↑ Lua error in package.lua at line 80: module 'strict' not found.
  6. ↑ 6.0 6.1 Lua error in package.lua at line 80: module 'strict' not found.
  7. ↑ 7.0 7.1 Lua error in package.lua at line 80: module 'strict' not found.
  8. ↑ Lua error in package.lua at line 80: module 'strict' not found.
  9. ↑ 9.0 9.1 Lua error in package.lua at line 80: module 'strict' not found.
  10. ↑ 10.0 10.1 Lua error in package.lua at line 80: module 'strict' not found.
  11. ↑ Lua error in package.lua at line 80: module 'strict' not found.
  12. ↑ Lua error in package.lua at line 80: module 'strict' not found.

External links

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