RX J0806.3+1527

From Wikipedia, the free encyclopedia
RX J0806.3+1527
J0806 (binary star - artist's conception).jpg
An artist's depiction of J0806.
Observation data
Epoch J2000      Equinox J2000
Constellation Cancer
Right ascension 08h 06m 22.95196s[1]
Declination +15° 27′ 31.0073″[1]
Distance 1,600 Light-years
Binary orbit
Period (P) 321.5 seconds
(Pdot) 1.1 milliseconds per year
Separation: 0.0005 AU
Details
Mass0.5 (primary) / 0.5 (b) M☉
Other designations
RX J0806.3+1527, RX J0806, J0806, HM Cancri, HM Cnc
Database references
SIMBADdata

RX J0806.3+1527 or HM Cancri (sometimes shortened to HM Cnc or J0806 after establishing identity) is an X-ray binary star system about 1,600 light-years (490 pc; 1.5×1016 km) away.[2] It comprises two dense white dwarfs orbiting each other once every 321.5 seconds (in this system the "year" duration is of only 5.4 minutes), at an estimated distance of only 80,000 kilometres (50,000 mi) apart (about 1/5 the distance between the Earth and the Moon). The two stars orbit each other at speeds in excess of 400 kilometres per second (890,000 mph). The stars are estimated to be about half as massive as the Sun. Like typical white dwarfs, they are extremely dense, being composed of degenerate matter, and so have radii on the order of the Earth's radius. Astronomers believe that the two stars will eventually merge, based on data from many X-ray satellites, such as Chandra X-Ray Observatory, XMM-Newton and the Swift Gamma-Ray Burst Mission. These data show that the orbital period of the two stars is steadily decreasing at a rate of 1.2 milliseconds per year as they thus are getting closer by approximately 60 centimetres (2.0 ft) per day. At this rate, they can be expected to merge in approximately 340,000 years. With a revolution period of 5.4 minutes, RX J0806.3+1527 is the shortest orbital period binary system currently known.

Observations[]

As RX J0806.3+1527 is a pair of white dwarfs, it has a relatively low optical luminosity. The 321.5 s modulation of RX J0806.3+1527 was discovered serendipitously in 1999 thanks to the ROSAT mission working in the X-ray band. Optical follow-up observations with the ESO Very Large Telescope (VLT), Telescopio Nazionale Galileo (TNG) and Nordic Optical Telescope (NOT) allowed the counterpart to be identified, a relatively dim (20.7 magnitude in the B filter) object which shows an optical modulation at the same period detected in the X-ray band. The optical monitoring of the counterpart of RX J0806.3+1527 during 2001-2004 clearly shows that the period is decreasing at a rate of about 1/1000 s each year. This result was confirmed by monitoring the source in the X-rays for several years.

Relation to general relativity[]

The decreasing separation of the components of the system mean that the system is losing orbital energy. Albert Einstein's theory of General Relativity predicts such a system will lose orbital energy through the generation of gravitational waves. Scientists believe that RX J0806.3+1527 may be one of the strongest sources of gravitational waves in the Milky Way galaxy.[citation needed]

Sources[]

  1. ^ Jump up to: a b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ "RX J0806.3+1527: Orbiting Stars Flooding Space with Gravitational Waves". CHANDRA X-RAY OBSERVATORY, Harvard. 2005-05-30. Archived from the original on 2005-05-30. Retrieved 2013-05-31.

Further reading[]

Retrieved from ""