PSR J1719−1438: Difference between revisions
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'''PSR J1719-1438''' is a [[millisecond pulsar]] with a spin period of 5.7 ms located about 4000 ly from Earth in the direction of [[Serpens]] Cauda, |
'''PSR J1719-1438''' is a [[millisecond pulsar]] with a spin period of 5.7 ms located about 4000 [[light year|ly]] from Earth in the direction of [[Serpens]] Cauda,<ref name=bailes/><ref name=UniverseToday /> approximately one [[Minute of arc|minute]] from the border with Ophiuchus. Millisecond pulsars are generally thought to begin as normal pulsars and then spin up by accreting matter from a binary companion. |
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==Diamond planet== |
==Diamond planet== |
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Revision as of 18:30, 27 September 2011
| Observation data Epoch MJD 55411.0[1] Equinox J2000 | |
|---|---|
| Constellation | |
| Right ascension | 17:19:10.0730(1)[1] |
| Declination | −14:38:00.96(2)[1] |
| Characteristics | |
| Spectral type | millisecond pulsar[1] |
| Apparent magnitude (R) | >25.4[1] |
| Apparent magnitude (g) | >24.1[1] |
| Apparent magnitude (I) | >22.5[1] |
| Astrometry | |
| Distance | ~1,200[1] pc |
| Orbit[1] | |
| Primary | PSR J1719-1438 |
| Companion | PSR J1719-1438b |
| Period (P) | 0.090706293(2) days |
| Semi-major axis (a) | 0.001819(1) light seconds |
| Eccentricity (e) | <0.06 |
| Periastron epoch (T) | MJD 55411.0 |
| Details | |
| Other designations | |
| Database references | |
PSR J1719-1438 is a millisecond pulsar with a spin period of 5.7 ms located about 4000 ly from Earth in the direction of Serpens Cauda,[1][2] approximately one minute from the border with Ophiuchus. Millisecond pulsars are generally thought to begin as normal pulsars and then spin up by accreting matter from a binary companion.
Diamond planet
PSR J1719-1438 was discovered in 2010 by the High Time Resolution Survey, a radio astronomy search for astronomical objects which rapidly vary in radio brightness, such as pulsars.[1] Timing measurements using the Parkes Telescope and Lovell Telescope showed that it has a low-mass companion: PSR J1719-1438 b.[1] The companion has a mass similar to that of Jupiter, but at about 40% of the diameter. It orbits the pulsar with a period of 2.17 hours at a distance of around 600,000 km (0.89 solar radii).[1] The companion is likely the remnants of a star whose outer layers were siphoned off by the more massive pulsar. Calculations show the companion has a minimum density of 23 grams per cubic centimeter and is probably a ultra-low mass carbon-oxygen white dwarf.[1]
Because the companion to PSR J1719-1438 is planet sized, made primarily of carbon (with an unknown amount of oxygen), and is very dense, it may be similar to a very large diamond. In the science press, the object has been called the "Diamond Planet"[2][3][4].
See also
- EF Eridani, a star system with a compact star and a degraded planetary-mass former star
References
- ^ a b c d e f g h i j k l m n Bailes, M.; Bates, S. D.; Bhalerao, V.; Bhat, N. D. R.; Burgay, M.; Burke-Spolaor, S.; d'Amico, N.; Johnston, S.; Keith, M. J. (2011). "Transformation of a Star into a Planet in a Millisecond Pulsar Binary". Science. doi:10.1126/science.1208890.
- ^ a b "Star Transforms Into A Diamond Planet". Universe Today. Retrieved 8/26/2011.
{{cite web}}: Check date values in:|accessdate=(help) - ^ "Surprise! Alien Planet Made of Diamond Discovered". Space.com. Retrieved 8/25/2011.
{{cite web}}: Check date values in:|accessdate=(help) - ^ "A Planet made of Diamond". Max Planck Institut for Radio Astronomy. Retrieved 8/26/2011.
{{cite web}}: Check date values in:|accessdate=(help)