HR 753
| HR 753 | |
|---|---|
| Pozorovací údaje (Ekvinokcium J2000,0) | |
| Typ | trojhvězda |
| Souhvězdí | Velryba |
| Vzdálenost | 7,18 pc |
| Označení v katalozích | |
| 2MASS | 2MASS J02360498+0653140 a 2MASS J02361535+0652191 |
| IRAS | IRAS 02334+0639 |
| (V) – měření provedena ve viditelném světle | |
| Některá data mohou pocházet z datové položky. | |
HR 753 je hvězda spektrálního typu K3, vzdálená necelých 23,6 ly. Jedná se o červeného trpaslíka. Nachází se v souhvězdí Velryby. Radiální rychlost hvězdy činí přibližně 23,5 km/s.
Reference
V tomto článku byly použity překlady textů z článků HR 753 na slovenské Wikipedii, HR 753 na nizozemské Wikipedii a Gliese 105 na italské Wikipedii.
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Obrázky, zvuky či videa k tématu HR 753 na Wikimedia Commons
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Gliese 105.gif
Is the dim star to the upper right of this false-color picture the coolest possible normal star? From this recent picture by the Hubble Space Telescope, astronomers have estimated its mass is just high enough for it to fuse hydrogen into helium in its core. In general, the higher an object's mass, the higher it's core density and temperature. Above a certain point, the intense core conditions cause hydrogen atoms to move so fast that many stick or "fuse" after collision, releasing enormous amounts of energy. Were this object less massive, the object would shine by gravitational contraction and so be termed a "brown dwarf" rather than a normal main-sequence "star." The star on the left is so much brighter than the "coolest star" that it creates the white streak and dramatic pattern visible in the image.
Is the dim star to the upper right of this false-color picture the coolest possible normal star? From this recent picture by the Hubble Space Telescope, astronomers have estimated its mass is just high enough for it to fuse hydrogen into helium in its core. In general, the higher an object's mass, the higher it's core density and temperature. Above a certain point, the intense core conditions cause hydrogen atoms to move so fast that many stick or "fuse" after collision, releasing enormous amounts of energy. Were this object less massive, the object would shine by gravitational contraction and so be termed a "brown dwarf" rather than a normal main-sequence "star." The star on the left is so much brighter than the "coolest star" that it creates the white streak and dramatic pattern visible in the image.