WISE 1541–2250 (full designation - WISEPA J154151.66-225025.2 ) is a brown dwarf rather close to the Sun that is in the constellation Libra .
| WISE 1541-2250 | |||
|---|---|---|---|
| Star | |||
 WISE 1541-2250 in the view of the artist. | |||
| Observational data ( Epoch J2000.0 ) | |||
| Right ascension | |||
| Declination | |||
| Distance | 18.6 sv. years (5.7 pc ) | ||
| Visible magnitude ( V ) | 20.99 | ||
| Constellation | Libra | ||
| Astrometry | |||
| Proper motion (μ) | RA: -870 mas per year Dec: -13 mas per year | ||
| Parallax (π) | 175.1 ± 4.4 mas | ||
| Absolute magnitude (V) | +22.21 | ||
| Specifications | |||
| Spectral class | Y0.5 | ||
| physical characteristics | |||
| Weight | 0,008—0,012 M ☉ | ||
| Radius | 1.01–1.07 R ☉ | ||
| Temperature | 350 K | ||
| Luminosity | 1.116 * 10 ^ -7 L ☉ | ||
| |||
| Information in databases | |||
| SIMBAD | |||
Content
Distance
In 2013, a trigonometric parallax of 87 ± 54 mas [2] was published, which corresponds to a distance of 11.5 parsec (37.5 light years) and 0.021 ± 0.09 angular seconds, which corresponds to a distance of> 6.0 parsec (> 19.6 St. years) [3] . Later parallax was refined - first to 74 ± 31 mas (13.5 light years or 4.0 pc) [4] , and then - 175.1 ± 4.4 mas.
Upon discovery, it was assumed that WISE 1541-2250 is the closest known brown dwarf located about 9 light years from the Sun, that is, more than two times farther than the distance to the nearest Alpha Centauri star system. WISE 1541-2250 is in seventh place in the list of stars closest to the Sun. According to another estimate, it was assumed that WISE 1541-2250 is located at a distance of 5.9 light years from Earth, that is, slightly closer than the Barnard Star [5] . In 2012, the star's parallax was equal to 0.087 ± 0.054, which corresponds to a distance of 11.5 +18.8
−4.4 parsecs or 37.5 +61.3
−14.4 light years (that is, no closer than 23.1 light years). However, due to a very large error, Kirkpatrick and his colleagues questioned these data and estimated the distance to the star according to spectrophotometry at 4.2 parsec (13.7 light years) [6] . In 2014, parallax was defined as 176 ± 9 mas and 175.1 ± 4.4 mas (5.7 pc, 18.6 years old) and it was assumed that this is a binary system [7] .
Physical parameters
WISE 1541-2250 belongs to the spectral class Y0 and has a surface temperature of about 350 K. The radius of the brown dwarf is 1.01-1.07 of the radius of Jupiter, and the mass is 8-12 masses of Jupiter. WISE 1541-2250 is one of six cold brown dwarfs, of spectral class Y (along with WISE 0410 + 1502 , WISE 1405 + 5534 , WISE 1738 + 2732 , WISE 1828 + 2650 and WISE 2056 + 1459 ), discovered in 2011 by infrared space telescope Wide-field Infrared Survey Explorer (WISE) [8] . Its habitable zone is located only 50,000 km from the surface [9] . However, no brown dwarf planet was found.
See also
- List of nearby stars
- SO 02353 + 1652 - 12.5 + 0.1 / -0.1 st. years old
- SCR 1845-6357 A - 12.6 + 0.1 / -0.1 st. years old
- SCR 1845-6357 B - 12.6 + 0.7 / -0.7 st. years old
- UGPS 0722−05 - 13.4 St. years old
- DEN 0817-6155 - 16.0 + 1 / -1 st. years old
- DEN 0255-4700 - 16.2 + 0.3 / -0.3 st. years old
- LHS 1723 - 17.4 + 0.1 / -0.1 st. years old
- G 099-049 - 17.6 + 1.0 / -1.0 st. years old
- WISE J1741 + 2553 - 18 + 2 / -2 st. years old
- 2MASS 1835 + 3259 - 18.5 + 0.05 / -0.05 h. years old
- 2MASS 0415-0935 - 18.6 + 0.2 / -0.2 st. years old
- 2MASS 0937 + 2931 - 20.0 + 0.2 / -0.2 st. years old
- WISE J0254 + 0223 - 24 St. years old
- SIPS 1259-4336 - 25.8 + 0.2 / -0.2 st. years old
Notes
- ↑ Kirkpatrick, J. Davy & Cushing; Gelino; Griffith; Skrutskie; Marsh; Wright; Mainzer; Eisenhardt; McLean; Thompson; Bauer; Benford; Bridge; Lake; Petty; Stanford; Tsai; Bailey; Beichman; Bochanski; Burgasser; Capak; Cruz; Hinz; Kartaltepe; Knox; Manohar; Masters; Morales-Calderónn; Prato; Rodigas; Salvato; Schurr; Scoville; Simcoe; Stapelfeldt; Stern; Stock; Vacca (2011), "The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE)", arΧiv : 1108.4677v1 [astro-ph.SR]
- ↑ Kirkpatrick, J. Davy; Gelino, Christopher R .; Cushing, Michael C .; Mace, Gregory N .; Griffith, Roger L .; Skrutskie, Michael F .; Marsh, Kenneth A .; Wright, Edward L .; Eisenhardt, Peter R .; McLean, Ian S .; Mainzer, Amanda K .; Burgasser, Adam J .; Tinney, CG; Parker, Stephen; Salter, Graeme (2012). “Further Defining Spectral Type“ Y “and Exploring the Low End Brown Field Mass Function.” The Astrophysical Journal 753 (2): 156.
- Net Kenneth A. Marsh, Edward L. Wright, J. Davy Kirkpatrick, Christopher R. Gelino, Michael C. Cushing, Roger L. Griffith, Michael F. Skrutskie, Peter R. Eisenhardt. Brown Dwarfs of Spectral Types Y and Late T
- ↑ Dupuy, Trent J.; Kraus, Adam L. (2013). "Distances, Luminosities, Substellar Objects Coldest Known Substellar Objects"
- ↑ Cushing, Michael C. & Kirkpatrick; Gelino; Griffith; Skrutskie; Mainzer; Marsh; Beichman; Burgasser; Prato; Simcoe; Marley; Saumon; Freedman; Eisenhardt; Wright (2011), "THE DISCOVERY OF Y DWARFS USING DATA FROM THE WIDE-FIELD INFRARED SURVEY EXPLORER (WISE)", ArΧiv : 1108.4678v1 [astro-ph.SR]
- ↑ Kirkpatrick, J. Davy; Gelino, Christopher R .; Cushing, Michael C .; Mace, Gregory N .; Griffith, Roger L .; Skrutskie, Michael F .; Marsh, Kenneth A .; Wright, Edward L .; Eisenhardt, Peter R .; McLean, Ian S .; Mainzer, Amanda K .; Burgasser, Adam J .; Tinney, CG; Parker, Stephen; Salter, Graeme (2012). “Further Defining Spectral Type“ Y “and Exploring the Low End Brown Field Mass Function”
- ↑ The Luminosities of the Coldest Brown Dwarfs (inaccessible link - history ) .
- ↑ Gelino & Kirkpatrick; Cushing; Eisenhardt; Griffith; Mainzer; Marsh; Skrutskie; Wright (2011), "WISE Brown Dwarf Binaries: The Discovery of the T5 + T5 and a T8.5 + T9 System", arΧiv : 1106.3142v1 [astro-ph.SR]
- ↑ Zone of habitability (rus.) // Wikipedia. - 2016-09-06.