V450 Scuti is a red supergiant and a semiregular variable star located in the constellation Scutum. Its apparent magnitude varies between 5.37 and 5.6m, which makes it visible to the naked eye under dark skies. The distance to V450 Scuti is uncertain, with estmates ranging from 1,270 to 4,100 light-years from Earth. It is moving away from Earth at a velocity of 4.9 km/s.
Characteristics edit
V450 Scuti has a spectral type of K3Iab,[1] meaning that is a K-type red supergiant star with an intermediate luminosity. It is 12.6 times more massive than the Sun[1] and has expanded to 321 times the Sun's size.[2] The star is emitting 25,700 times the solar luminosity from its photosphere at an effective temperature of 4,080 K,[2] which is signifcantly cooler than the Sun's photosphere. Despite its advanced evolutionary stage, the age of V450 Scuti is of only 17.6 million years,[1] which is about 1/260 of the solar age of 4.6 billion years. It happens because massive stars (such as V450 Scuti) exhausts their hydrogen supplement much faster than the Sun, and therefore evolve much faster.[3] When this star reaches the end of its life, it will explode in a supernova, thus producing a neutron star remnant.[3] The B-V color index of this star is 1.97, giving it the red hue of a M-type star. This is much redder than expected for a K-type star, and it caused by a
Distance edit
The distance to V450 Scuti is uncertain, with different sources giving different distances, all with significsnt uncertainites. Gaia DR3 (2023) measured a parallax of 0.7958±0.2518 mas for V450 Scuti, translating into a distance of 1,256.6±397.6 parsecs (4,096.5±1,296 ly).[4] This parallax, however, has a very high significance of astrometric noise of 615 (anything above 2 is probable significant), thus causing a discrepancy in the parallax's angular measure and affecting its reliability.[4][5] Gaia DR2 (2018) measured a parallax of 1.8422±0.3651 mas, giving it a distance of 542.8±107.6 pc (1770±351 ly).[6] This parallax has also a high significancr of astrometric noise, rated at 222.[6]
A 2012 paper gives a distance of 885±283 pc (2885±923 ly) for this star, which has an uncertainity of 0.32.[7] Another paper from 2010 gives a parallax of 1.157±0.371 mas, translating into a distance of 864±277 pc (2817±903 ly).[8] The Hipparcos spacecraft (2007) measured a parallax of 2.57±0.77 mas, which translate into a distance of 389.1±116.6 pc (1268±380 ly).[9]
| Paper | Parallax (mas) |
Distance (parsecs) |
Distance (light-years) |
Ref |
|---|---|---|---|---|
| Gaia DR3 (2023) |
0.7958±0.2518 | 1,256.6±397.6 | 4,096.5±1,296 | [5] |
| Gaia DR2 (2018) |
1.8422±0.3651 | 542.8±107.6 | 1770±351 | [6] |
| McDonald et al. (2012) |
– | 885±283 | 2885±923 | [7] |
| Hohle et al. (2010) |
1.157±0.371 | 864±277 | 2817±903 | [8] |
| Hipparcos (2007) |
2.57±0.77 | 389.1±116.6 | 1268±380 | [9] |
Notes edit
References edit
- ^ a b c Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (2011-01-01). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society. 410: 190–200. doi:10.1111/j.1365-2966.2010.17434.x. ISSN 0035-8711.
- ^ a b Hohle, M. M.; Neuhäuser, R.; Schutz, B. F. (2010-04-01). "Masses and luminosities of O- and B-type stars and red supergiants". Astronomische Nachrichten. 331: 349. doi:10.1002/asna.200911355. ISSN 0004-6337.
- ^ a b "Red Supergiant Stars". hyperphysics.phy-astr.gsu.edu. Retrieved 2024-05-09.
- ^ a b Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b Lindegren, L.; Klioner, S. A.; Hernández, J.; Bombrun, A.; Ramos-Lerate, M.; Steidelmüller, H.; Bastian, U.; Biermann, M.; de Torres, A.; Gerlach, E.; Geyer, R.; Hilger, T.; Hobbs, D.; Lammers, U.; McMillan, P. J. (2021-05). "Gaia Early Data Release 3: The astrometric solution". Astronomy & Astrophysics. 649: A2. doi:10.1051/0004-6361/202039709. ISSN 0004-6361.
{{cite journal}}: Check date values in:|date=(help) - ^ a b c 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.
- ^ a b McDonald, I.; Zijlstra, A. A.; Boyer, M. L. (2012-11-01). "Fundamental parameters and infrared excesses of Hipparcos stars". Monthly Notices of the Royal Astronomical Society. 427: 343–357. doi:10.1111/j.1365-2966.2012.21873.x. ISSN 0035-8711.
- ^ a b Hohle, M. M.; Neuhäuser, R.; Schutz, B. F. (2010-04-01). "Masses and luminosities of O- and B-type stars and red supergiants". Astronomische Nachrichten. 331: 349. doi:10.1002/asna.200911355. ISSN 0004-6337.
- ^ a b van Leeuwen, Floor (13 August 2007). "Validation of the new Hipparcos reduction". Astronomy & Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. eISSN 1432-0746. ISSN 0004-6361. Hipparcos record for this source at VizieR.