BD+14 4559 b

BD+14 4559 b
Exoplanet List of exoplanets

Artist's impression of BD+14 4559 b (foreground), depicted here as a gas giant planet with rings, orbiting its host star (center)
Parent star
Star BD+14 4559
Constellation Pegasus
Right ascension (α) 21h 13m 35.99s[1]
Declination (δ) +14° 41′ 21.8″[1]
Apparent magnitude (mV) 9.63
Distance158 ± 9[1] ly
(48 ± 3[1] pc)
Spectral type K2V[2]
Mass (m) 0.86 (± 0.15)[2] M☉
Radius (r) 0.95 (± 0.2)[2] R☉
Temperature (T) 5008 (± 20)[2] K
Metallicity [Fe/H] 0.10 (± 0.07)[2]
Age ~3 Gyr
Physical characteristics
Minimum mass(m sin i)1.47 MJ
(467.46 M⊕)
Radius(r)~1.05 RJ
Stellar flux(F⊙)0.44 ⊕
Temperature (T) 205 K (−68 °C; −91 °F)
Orbital elements
Semi-major axis(a) 0.777 AU
Periastron (q) 0.552 AU
Apastron (Q) 1.002 AU
Eccentricity (e) 0.29 ± 0.03
Orbital period(P) 268.94 ± 0.99 d
Argument of
periastron		 (ω) 87.64 ± 7.87°
Time of periastron (T0) 53293.71 ± 6.35 JD
Discovery information
Discovery date June 10, 2009
Discoverer(s) Niedzielski et al.
Discovery method radial velocity
Discovery site La Silla Observatory
Discovery status Published
Database references
Extrasolar Planets
Encyclopaedia		data
SIMBADdata
Exoplanet Archivedata
Open Exoplanet Cataloguedata

BD+14 4559 b is an exoplanet orbiting the K-type main sequence star BD+14 4559 about 158 light-years (48 parsecs, or nearly 1.5×1015 km) from Earth in the constellation Pegasus. It orbits its star within the habitable zone at a distance of 0.777 AU, close to that of Venus, but its star is less energetic, thus its habitable zone is closer to it than Earth. 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.[2]

Characteristics

Mass, radius and temperature

BD+14 4559 b is a gas giant, an exoplanet that has a radius and mass around that of the gas giants Jupiter and Saturn. It has a temperature of 205 K (−68 °C; −91 °F).[3] It has an estimated mass of around 1.2 MJ and a potential radius of around 1.05 RJ based on its mass.

Host star

The planet orbits a (K-type) star named BD+14 4559. The star has a mass of 0.86 M☉ and a radius of around 0.95 R☉. It has a surface temperature of 5008 K and is likely about 3 billion years old based on its evolution and mass. In comparison, the Sun is about 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 9.63. Therefore, BD+14 4559 is too dim to be seen with the naked eye, but can be viewed using good binoculars.

Orbit

BD+14 4559 b orbits its star with about 25% of the Sun's luminosity every 268 days at a distance of 0.77 AU (close to Venus's orbital distance from the Sun, which is 0.72 AU). It has a mildly eccentric orbit, with an eccentricity of 0.29.

Habitability

BD+14 4559 b resides in the habitable zone of the parent star. The exoplanet, with a mass of 1.47 MJ, is too massive to likely be rocky, and because of this the planet itself may not be 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.

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.[6][7] 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.[8] In the case of BD+14 4559 b, the orbital period would have to be no greater than a month (28–29 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[9][10] and create a geodynamo effect which would give the satellite a strong magnetic field.[11]

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⊕.[12] 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⊕.[8]

Discovery

The search for BD+14 4559 b started when its host star was chosen an ideal target for a planet search using the radial velocity method (in which the gravitational pull of a planet on its star is measured by observing the resulting Doppler shift), as stellar activity would not overly mask or mimic Doppler spectroscopy measurements. It was also confirmed that BD+14 4559 is neither a binary star nor a quickly rotating star, common false positives when searching for transiting planets. Analysis of the resulting data found that the radial velocity variations most likely indicated the existence of a planet.[2] The net result was an estimate of a 1.47 MJ planetary companion orbiting the star at a distance of 0.77 AU with an eccentricity of 0.29.

Radial velocity measurements of BD+14 4559 were measured at 43 epochs over the period of roughly 1,265 days (around 4 years) using the Hobby–Eberly Telescope.[2] Measurements determined that a signal-to-noise ratio per resolution element was around 150–260 at 594 nm in 10 to 25 minutes of integration. The estimated mean RV uncertainty for the parent star was estimated at 8 m s−1.

The discovery of BD+14 4559 b was reported in the journal The Astrophysical Journal on June 10, 2009.

See also

References

  1. 1 2 3 4 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. 1 2 3 4 5 6 7 8 Niedzielski, A.; et al. (2009). "Substellar-mass Companions to the K-dwarf BD+14 4559 and the K-giants HD 240210 and BD+20 2457". The Astrophysical Journal. 707 (1): 768–777. arXiv:0906.1804. Bibcode:2009ApJ...707..768N. doi:10.1088/0004-637X/707/1/768.
  3. ↑ http://www.hpcf.upr.edu/~abel/phl/hec_plots/hec_orbit/hec_orbit_BD14_4559_b.png
  4. ↑ Fraser Cain (16 September 2008). "How Old is the Sun?". Universe Today. Retrieved 19 February 2011.
  5. ↑ Fraser Cain (September 15, 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: 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.
  8. 1 2 Andrew J. LePage. "Habitable Moons:What does it take for a moon — or any world — to support life?". SkyandTelescope.com. Retrieved 2011-07-11.
  9. ↑ Glatzmaier, Gary A. "How Volcanoes Work – Volcano Climate Effects". Retrieved 29 February 2012.
  10. ↑ "Solar System Exploration: Io". Solar System Exploration. NASA. 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.

Coordinates: 21h 13m 35.99s, +14° 41′ 21.8″

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