HD 69830

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HD 69830
Morgan-Keenan spectral classification zoom.png

HD 69830 is a K0V class star less massive than the Sun (G2V)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Puppis
Right ascension 08h 18m 23.947s[1]
Declination −12° 37′ 55.81″[1]
Apparent magnitude (V) +5.95
Characteristics
Spectral type K0V
U−B color index 0.34
B−V color index 0.753
V−R color index 0.40
R−I color index 0.36
Variable type none
Astrometry
Radial velocity (Rv) +30.4 km/s
Proper motion (μ) RA: 278.99 ± 0.25[1] mas/yr
Dec.: −987.59 ± 0.29[1] mas/yr
Parallax (π) 80.04 ± 0.35[1] mas
Distance 40.7 ± 0.2 ly
(12.49 ± 0.05 pc)
Absolute magnitude (MV) 5.47 ± 0.01[2]
Details
Mass 0.86 ± 0.03 M
Radius 0.89 R
Luminosity 0.60 ± 0.03 L
Surface gravity (log g) 4.47 cgs
Temperature 5385 ± 20 K
Metallicity 89 ± 4 %
Rotation 35.1 ± 0.8 days[3]
Age (5.1–6.1) × 109[4] years
Other designations
285 G. Puppis,[5] HR 3259, GJ 302, HIP 40693, SAO 154093, LHS 245, BD−12°2449
Database references
SIMBAD data
Exoplanet Archive data
ARICNS data
Extrasolar Planets
Encyclopaedia
data

HD 69830 (285 G. Puppis) is an orange dwarf star approximately 41 light-years away in the constellation of Puppis. In 2005, the Spitzer Space Telescope discovered a debris disk orbiting the star.[6] The disk contains substantially more dust than the Solar System's asteroid belt. As of 2006, it has been confirmed that three extrasolar planets with minimum masses comparable to Neptune orbit the star, located interior to the debris disk.[7]

Distance and visibility[edit]

HD 69830 is an orange dwarf star of the spectral type K0V. The star has a mass of about 86 percent the Sun, 89 percent of its radius, and 45 percent of its luminosity. Containing 11 percent less iron than the Sun, recent age estimates indicated that the star is about 7 billion years old. HD 69830 is located about 41.0 light-years from the Sun, lying in the northeastern part of the constellation of Puppis (the Poop Deck). The star can be found east of Sirius, southwest of Procyon, northeast of Delta Canis Majoris, and north of Zeta Puppis.

Planetary system[edit]

The orbits of the planets of HD 69830 and the debris disk.
The HD 69830 planetary system[7][8]
Companion
(in order from star)
Mass Semimajor axis
(AU)
Orbital period
(days)
Eccentricity Inclination Radius
b ≥10.48 M 0.0785 8.667 ± 0.003 0.1 ± 0.04
c ≥12.07 M 0.186 31.56 ± 0.04 0.13 ± 0.06
d ≥18.43 M 0.63 197 ± 3 0.07 ± 0.07
Asteroid belt 0.93–1.16 AU

Debris disk[edit]

A comparison between the night sky of Earth and a body of HD 69830.

In 2005, the Spitzer Space Telescope detected a debris disk in the HD 69830 system consistent with being produced by an asteroid belt twenty times more massive than that in our own system. The belt was originally thought to be located inside an orbit equivalent to that of Venus in our own Solar System, which would place it between the orbits of the second and third planets. The disk contains sufficient quantities of dust that the nights on any nearby planets would be lit up by zodiacal light 1000 times brighter than that seen on Earth, easily outshining the Milky Way.

Further analysis of the spectrum of the dust revealed that it is composed of highly processed material, likely derived from a disrupted C-type asteroid of at least 30 km radius which contained many small olivine-rich (rocky) and once-wet grains which would not survive at close distances to the star. Instead, it seems more likely that the asteroid belt producing the dust is located outside the orbit of the outermost planet, around 1 AU from the star. This region contains the 2:1 and 5:2 mean motion resonances with HD 69830 d.[8]

Planets[edit]

Artist's impression from 2005 of the asteroid belt and a hypothetical outer planet.

On May 17, 2006, a team of astronomers using the European Southern Observatory's (ESO) HARPS spectrograph on the 3.6-metre La Silla telescope in the Atacama desert, Chile, announced the discovery of three extrasolar planets orbiting the star. With minimum masses between 10 to 18 times that of the Earth, all three planets are presumed to be similar to the planets Neptune or Uranus. As of 2011, no planet with more than half the mass of Jupiter had been detected within three astronomical units of HD 69830.

The star rotates at an inclination of 13+27
−13
degrees relative to Earth.[3] It has been assumed that the planets share that inclination.[9] However b and c are "hot Neptunes", and outside this system several are now known to be oblique relative to the stellar axis.[10]

The outermost planet discovered appears to be within the system's habitable zone, where liquid water would remain stable (more accurate data on the primary star's luminosity will be required to know for sure where the habitable zone is). HD 69830 is the first extrasolar planetary system around a Sun-like star without any known planets comparable to Jupiter or Saturn in mass.

References in popular culture[edit]

  • In the Bestiarum included with the special editions of Halo 3, it declares Eayn, a satellite of HD 69830 d as the home of the Jackals, specifically stating they come from the moon of the third planet, at the inner edge of the asteroid belt.

See also[edit]

References[edit]

  1. ^ a b c d e van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. Vizier catalog entry
  2. ^ Holmberg, J. et al. (2009). "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics". Astronomy and Astrophysics 501 (3): 941–947. arXiv:0811.3982. Bibcode:2009A&A...501..941H. doi:10.1051/0004-6361/200811191. Vizier catalog entry
  3. ^ a b Simpson, E. K. et al. (November 2010), "Rotation periods of exoplanet host stars", Monthly Notices of the Royal Astronomical Society 408 (3): 1666–1679, arXiv:1006.4121, Bibcode:2010MNRAS.408.1666S, doi:10.1111/j.1365-2966.2010.17230.x 
  4. ^ Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008). "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics". The Astrophysical Journal 687 (2): 1264–1293. arXiv:0807.1686. Bibcode:2008ApJ...687.1264M. doi:10.1086/591785. 
  5. ^ Benjamin Apthorp Gould, reprinted and updated by Frederick Pilcher. "Uranometria Argentina". Retrieved 2011-02-04. 
  6. ^ Beichman, C. A. et al. (2005). "An Excess Due to Small Grains around the Nearby K0 V Star HD 69830: Asteroid or Cometary Debris?". The Astrophysical Journal 626 (2): 1061–1069. arXiv:astro-ph/0504491. Bibcode:2005ApJ...626.1061B. doi:10.1086/430059. 
  7. ^ a b Lovis, Christophe et al. (2006). "An extrasolar planetary system with three Neptune-mass planets" (PDF). Nature 441 (7091): 305–309. arXiv:astro-ph/0703024. Bibcode:2006Natur.441..305L. doi:10.1038/nature04828. 
  8. ^ a b Lisse, C. M. et al. (2007). "On the Nature of the Dust in the Debris Disk Around HD 69830". The Astrophysical Journal 658 (1): 584–592. arXiv:astro-ph/0611452. Bibcode:2007ApJ...658..584L. doi:10.1086/511001. 
  9. ^ "hd_69830_b". Extrasolar Planet Encyclopaedia. Retrieved November 12, 2012. 
  10. ^ Roberto Sanchis-Ojeda, Josh N. Winn, Daniel C. Fabrycky (2012). Starspots and spin-orbit alignment for Kepler cool host stars. arXiv:1211.2002. Bibcode:2013AN....334..180S. doi:10.1002/asna.201211765. 

External links[edit]

Coordinates: Sky map 08h 18m 23.9s, −12° 37′ 55.0″