HD 69830 d

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HD 69830 d
Exoplanet List of exoplanets
HD 69830 System.jpg
Artist's impression of the HD 69830 system as viewed from planet "d" (foreground).
Parent star
Star HD 69830
Constellation Puppis
Right ascension (α) 08h 18m 23.947s[1]
Declination (δ) −12° 37′ 55.81″[1]
Apparent magnitude (mV) 5.98
Distance 40.7 ± 0.2[1] ly
(12.49 ± 0.05[1] pc)
Spectral type G8V[2]
Mass (m) 0.86 (± 0.04)[2] M
Radius (r) 0.905 (± 0.019)[2] R
Temperature (T) 5394 (± 62)[2] K
Metallicity [Fe/H] −0.04 (± 0.03)[2]
Age 10.6 (± 4)[2] Gyr
Physical characteristics
Mass (m) 18.1 M
Radius (r) ~4 R
Temperature (T) 284 K (11 °C; 52 °F)
Orbital elements
Semi-major axis (a) 0.63 AU
Eccentricity (e) 0.07 (± 0.07)
Orbital period (P) 197 (± 3) d
Argument of
(ω) 224 ± 61°
Time of periastron (T0) 24513358 ± 34 JD
Semi-amplitude (K) 2.20 ± 0.19 m/s
Discovery information
Discovery date May 18, 2006
Discoverer(s) Lovis et al.[3]
Discovery method Radial velocity
Discovery status Published[3]
Database references
Extrasolar Planets
Exoplanet Archive data
Open Exoplanet Catalogue data

HD 69830 d is an exoplanet likely orbiting within the habitable zone of the star HD 69830, the outermost of three such planets discovered in the system. It is located approximately 40.7 light-years (12.49 parsecs, or 3.8505×1014 km) from Earth in the constellation of Puppis. The exoplanet was found by using the radial velocity method, from radial-velocity measurements via observation of Doppler shifts in the spectrum of the planet's parent star.


Mass, radius and temperature[edit]

HD 69830 is a ice giant, with a mass and radius near that of the planets Uranus and Neptune, but smaller than that of the gas giants Jupiter and Saturn. Its temperature is 284 K (11 °C; 52 °F), close to that of Earth. The radius is not known, however given its mass of 17 M, which is around that of the planet Neptune, it likely has a radius of around 4 R. In other terms, it is basically a warmer version of Neptune.

Host star[edit]

The planet orbits a (G-type) star named HD 69830, orbited by total of three planets, of which HD 69830 d has the longest orbital period. The star has a mass of 0.86 M and a radius of 0.90 R.[2] It has a surface temperature of 5394 K and is 10.6 billion years old. In comparison, the Sun is 4.6 billion years old[4] and has a surface temperature of 5778 K.[5]

The star's apparent magnitude, or how bright it appears from Earth's perspective, is 5.47. Therefore, HD 69830 is visible to the naked eye.


The planet's orbit has a low orbital eccentricity, like most of the planets in the Solar System. The semimajor axis of the orbit is only 0.63 AU, similar to that of Venus. However, its star is less massive and energetic than the Sun (with a luminosity of 0.62 L), thereby putting the planet within its habitable zone.


HD 69830 d likely resides in the habitable zone of its parent star. The exoplanet, with an estimated mass of 17 M, is too massive to likely be rocky, and because of this the planet itself is not habitable. Hypothetically, large enough moons, with a sufficient atmosphere and pressure, may be able to support liquid water and potentially life. However, such moons do not usually form around planets, they would likely have to be captured from afar; e.g, a protoplanet running astray.[6]

For a stable orbit the ratio between the moon's orbital period Ps around its primary and that of the primary around its star Pp must be < 1/9, e.g. if a planet takes 90 days to orbit its star, the maximum stable orbit for a moon of that planet is less than 10 days.[7][8] Simulations suggest that a moon with an orbital period less than about 45 to 60 days will remain safely bound to a massive giant planet or brown dwarf that orbits 1 AU from a Sun-like star.[9] In the case of HD 69830 d, this would be around 22 days in order to have a stable orbit.

Tidal effects could also allow the moon to sustain plate tectonics, which would cause volcanic activity to regulate the moon's temperature[10][11] and create a geodynamo effect which would give the satellite a strong magnetic field.[12]

To support an Earth-like atmosphere for about 4.6 billion years (the age of the Earth), the moon would have to have a Mars-like density and at least a mass of 0.07 M.[13] One way to decrease loss from sputtering is for the moon to have a strong magnetic field that can deflect stellar wind and radiation belts. NASA's Galileo's measurements hints large moons can have magnetic fields; it found that Jupiter's moon Ganymede has its own magnetosphere, even though its mass is only 0.025 M.[9]


HD 69830 d was discovered in 2006 with the HARPS echelle spectrograph installed on the European Southern Observatory 3.6-meter telescope at La Silla Observatory, Chile.[3]

See also[edit]


  1. ^ a b c d 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. ^ a b c d e f g STELLAR PARAMETERS FOR HD 69830, A NEARBY STAR WITH THREE NEPTUNE MASS PLANETS AND AN ASTEROID BELT. Angelle Tanner, Tabetha S. Boyajian, Kaspar von Braun, Stephen Kane, John M. Brewer, Chris Farrington, Gerard T. van Belle, Charles A. Beichman, Debra Fischer, Theo A. ten Brummelaar, Harold A. McAlister, Gail Schaefer. 17 December 2014. Retrieved 17 July 2016.
  3. ^ a b c 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. PMID 16710412. 
  4. ^ Fraser Cain (16 September 2008). "How Old is the Sun?". Universe Today. Retrieved 19 February 2011. 
  5. ^ Fraser Cain (15 September 2008). "Temperature of the Sun". Universe Today. Retrieved 19 February 2011. 
  6. ^ Jonathan O'Callaghan (10 March 2015). "Alien moons could be more likely to host life than Earth-like planets, claims scientist". Daily Mail. Retrieved 17 June 2016. 
  7. ^ Kipping, David (2009). "Transit timing effects due to an exomoon". Monthly Notices of the Royal Astronomical Society 392: 181–189. arXiv:0810.2243. Bibcode:2009MNRAS.392..181K. doi:10.1111/j.1365-2966.2008.13999.x. Retrieved 22 February 2012. 
  8. ^ Heller, R. (2012). "Exomoon habitability constrained by energy flux and orbital stability". Astronomy & Astrophysics 545: L8. arXiv:1209.0050. Bibcode:2012A&A...545L...8H. doi:10.1051/0004-6361/201220003. ISSN 0004-6361. 
  9. ^ a b Andrew J. LePage. "Habitable Moons:What does it take for a moon — or any world — to support life?". SkyandTelescope.com. Retrieved 2011-07-11. 
  10. ^ Glatzmaier, Gary A. "How Volcanoes Work – Volcano Climate Effects". Retrieved 29 February 2012. 
  11. ^ "Solar System Exploration: Io". Solar System Exploration. NASA. Retrieved 29 February 2012. 
  12. ^ Nave, R. "Magnetic Field of the Earth". Retrieved 29 February 2012. 
  13. ^ "In Search Of Habitable Moons". Pennsylvania State University. Retrieved 2011-07-11. 

External links[edit]

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