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HD 69830 d

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Ice giant exoplanet orbiting HD 69830
HD 69830 d
Artist's impression of the HD 69830 system as viewed from planet "d" (foreground).
Discovery
Discovered byC. Lovis et al.
Discovery dateMay 18, 2006
Detection methodRadial velocity
Orbital characteristics
Semi-major axis0.622 ± 0.014 AU (93,000,000 ± 2,100,000 km)
Eccentricity0.080±0.071
Orbital period (sidereal)201.4±0.4 d
Time of periastron24513358 ± 34
Argument of periastron224 ± 61
Semi-amplitude2.20 ± 0.19
StarHD 69830
Physical characteristics
Mean radius~4 R🜨
Mass≥ 12.26+0.89
−0.88 ME
Temperature284 K (11 °C; 52 °F)

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 3.8505×10 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.

Characteristics

Mass, radius and temperature

HD 69830 d is a Neptune-sized planet with a minimum mass of at least 12 ME, and an estimated temperature of 284 K (11 °C; 52 °F).

Host star

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☉. 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 and has a surface temperature of 5778 K.

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.

Orbit

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 0.62 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.

Habitability

See also: Habitability of natural satellites

HD 69830 d likely resides in the habitable zone of its parent star. The exoplanet, with an estimated mass of 17 ME, 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.

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. 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. 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 and create a geodynamo effect which would give the satellite a strong magnetic field.

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 ME. 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 ME.

Discovery

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.

In popular culture

In the Halo video game series, Eayn, a fictional moon of HD 69830 d, is the homeworld of the Kig-Yar species, a member species of the enemy faction, the Covenant Empire. The planet was known to them as Chu’ot.

See also

References

  1. ^ 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. S2CID 4343578. Archived from the original (PDF) on 2016-03-03. Retrieved 2013-11-22.
  2. ^ Laliotis, Katherine; Burt, Jennifer A.; et al. (February 2023). "Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions". The Astronomical Journal. 165 (4): 176. arXiv:2302.10310. Bibcode:2023AJ....165..176L. doi:10.3847/1538-3881/acc067.
  3. Tanner, Angelle; Boyajian, Tabetha S.; von Braun, Kaspar; et al. (2015). "Stellar Parameters for Hd 69830, A Nearby Star with Three Neptune Mass Planets and an Asteroid Belt". The Astrophysical Journal. 800 (2): 115. arXiv:1412.5251. Bibcode:2015ApJ...800..115T. doi:10.1088/0004-637X/800/2/115. ISSN 1538-4357. S2CID 16097733.
  4. Cain, Fraser (16 September 2008). "How Old is the Sun?". Universe Today. Retrieved 19 February 2011.
  5. Cain, Fraser (15 September 2008). "Temperature of the Sun". Universe Today. Retrieved 19 February 2011.
  6. Kipping, David (2009). "Transit timing effects due to an exomoon". Monthly Notices of the Royal Astronomical Society. 392 (1): 181–189. arXiv:0810.2243. Bibcode:2009MNRAS.392..181K. doi:10.1111/j.1365-2966.2008.13999.x.
  7. 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. S2CID 118458061.
  8. ^ LePage, Andrew J. (August 1, 2006). "Habitable Moons". Sky & Telescope.
  9. Glatzmaier, Gary A. "How Volcanoes Work – Volcano Climate Effects". Archived from the original on 23 April 2011. Retrieved 29 February 2012.
  10. "Solar System Exploration: Io". Solar System Exploration. NASA. Archived from the original on 16 December 2003. Retrieved 29 February 2012.
  11. Nave, R. "Magnetic Field of the Earth". Retrieved 29 February 2012.
  12. "In Search Of Habitable Moons". Pennsylvania State University. Retrieved 2011-07-11.

External links

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