82 Eridani

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82 Eridani
Observation data
Epoch J2000
Constellation
(pronunciation)		 Eridanus
Right ascension 03h 19m 55.6505s[1]
Declination −43° 04′ 11.221″[1]
Apparent magnitude (V) 4.27[1]
Characteristics
Spectral type G8 V[1]
U-B color index +0.21[1]
B-V color index +0.71[1]
Variable type None
Astrometry
Radial velocity (Rv) +87.3[1] km/s
Proper motion (μ) RA: 3037.21[1] mas/yr
Dec.: 726.52[1] mas/yr
Parallax (π) 165.00 ± 0.55[1] mas
Distance 19.77 ± 0.07 ly
(6.06 ± 0.02 pc)
Absolute magnitude (MV) 5.35[2]
Details
Mass 0.97[2] M☉
Radius 0.92[3] R☉
Surface gravity (log g) 4.17[4]
Luminosity 0.62[5][6] L☉
Temperature 5,338[4] K
Metallicity [Fe/H] = -0.54[4]
Rotation 0.52 km/s[7]
Age 1.3 ±0.3 × 1010[8] years
Other designations

82 Eridani is a star about 20 light years away from Earth. It is in constellation Eridanus. It is a main sequence star of spectral type G5.

Contents

[edit] Observation

82 G. Eridani (often abbreviated "82 Eridani") is the 82nd star in Eridanus in the now-obscure catalog Uranometria Argentina. The Argentina catalog, compiled by the 19th-century astronomer Benjamin Gould, is a southern celestial hemisphere analog of the more famous Flamsteed catalog, and used a similar numbering scheme. 82 G. Eridani is one of the very few "G." stars still referred to as such.

[edit] Properties

In terms of luminosity, 82 G. Eridani is marginally dimmer than the Sun; about half as luminous as Tau Ceti or Alpha Centauri B. The projected equatorial rotation rate (vsini) is a leisurely 0.52 km/s, compared to 2 km/s for the Sun.[7]

82 G. Eridani is a high-velocity star—it is moving relatively quickly compared to the average—and hence is probably a member of Population II, generally older stars whose motions take them well outside the plane of the Milky Way. Like many other Population II stars, 82 G. Eridani is somewhat metal-deficient (though much less deficient than many), and is older than the Sun. It has a relatively high orbital eccentricity of 0.40 about the galaxy, ranging between 4.6 and 10.8 kiloparsecs from the core. The estimated age of this star is close to the age of the universe, so it was likely formed early in the history of the Milky Way.[8]

This star is located in a region of low-density interstellar matter (ISM), so it is believed to have a large astropause that subtends an angle of 6″ across the sky. Relative to the Sun, this star is moving at a space velocity of 101 km/s, with the bow shock advancing at more than Mach 3 through the ISM.[9]

[edit] Habitability

In his book Habitable Planets for Man,[10] Stephen Dole gave 82 G. Eridani his highest estimate for habitability: 5.7%. Four other stars had this figure: Alpha Centauri B, 70 Ophiuchi A, Eta Cassiopeiae A, and Delta Pavonis. 82 Eridani (GJ 139) was also picked as a Tier 1 target star for NASA's proposed Space Interferometry Mission (SIM) mission to search for Terrestrial-sized or larger planets.[11]

[edit] References

  1. ^ a b c d e f g h i j k SIMBAD Query Result: HD 20794 -- High proper-motion Star. Centre de Données astronomiques de Strasbourg. Retrieved on 2007-07-26.
  2. ^ a b Staff (June 8, 2007). List of the Nearest 100 Stellar Systems. Research Consortium on Nearby Stars (RECONS), Georgia State University. Retrieved on 2007-07-26.
  3. ^ Johnson, H. M.; Wright, C. D. (1983). "Predicted infrared brightness of stars within 25 parsecs of the sun". Astrophysical Journal Supplement Series 53: 643-711. doi:10.1086/190905.  — See the table on p. 653.
  4. ^ a b c Gratton, R. G. (1989). "Abundance of manganese in metal-poor stars". Astronomy and Astrophysics 208 (1-2): 171-178. 
  5. ^ Based upon:
    \frac{L}{L_{sun}} = \left ( \frac{R}{R_{sun}} \right )^2 \left ( \frac{T_{eff}}{T_{sun}} \right )^4
    where L is luminosity, R is radius and Teff is the effective temperature.
  6. ^ Krimm, Hans (August 19, 1997). Luminosity, Radius and Temperature. Hampden-Sydney College. Retrieved on 2007-05-16.
  7. ^ a b Santos, N. C. et al (2004). "Are beryllium abundances anomalous in stars with giant planets?". Astronomy and Astrophysics 427: 1085-1096. doi:10.1051/0004-6361:20040509. 
  8. ^ a b Hearnshaw, J. B. (1973). "The iron abundance of 82 Eridani". Astronomy and Astrophysics 29: 165-170. 
  9. ^ Frisch, P. C. (1993). "G-star astropauses - A test for interstellar pressure". Astrophysical Journal 407 (1): 198-206. 
  10. ^ Dole, Stephen H. (1970). Habitable Planets for Man, 2nd, London: American Elsevier Pub. Co. 0444000925. 
  11. ^ McCarthy, Chris (2005). SIM Planet Search Tier 1 Target Stars. San Francisco State University. Retrieved on 2007-07-26.

[edit] External links