HE 1523-0901: Difference between revisions
Aytosyrm D-B (talk | contribs) No edit summary Tag: Reverted |
GreenC bot (talk | contribs) Rescued 1 archive link. Wayback Medic 2.5 per WP:URLREQ#nbcnews.com |
||
| (5 intermediate revisions by 4 users not shown) | |||
| Line 2: | Line 2: | ||
{{Starbox begin}} |
{{Starbox begin}} |
||
{{Starbox image |
{{Starbox image |
||
| image = [[File: |
| image = [[File:He1523a.jpg|250px]] |
||
| ⚫ | |||
| caption = Example of a [[Binary star|binary star system]] (artist concept) |
|||
}} |
}} |
||
{{Starbox observe |
{{Starbox observe |
||
| Line 53: | Line 53: | ||
==Observation== |
==Observation== |
||
| ⚫ | |||
HE 1523-0901 is approximately 0.8 [[solar mass]]es, but the star has expanded until it is some 27 [[solar radius|times as large]], and has a [[bolometric luminosity|total luminosity]] of 730 times [[solar luminosity|that of the Sun]]. It can be viewed particularly well from the southern hemisphere with the use of a small telescope. It can also be observed from central European latitudes. |
HE 1523-0901 is approximately 0.8 [[solar mass]]es, but the star has expanded until it is some 27 [[solar radius|times as large]], and has a [[bolometric luminosity|total luminosity]] of 730 times [[solar luminosity|that of the Sun]]. It can be viewed particularly well from the southern hemisphere with the use of a small telescope. It can also be observed from central European latitudes. |
||
==Spectroscopic companion== |
==Spectroscopic companion== |
||
HE 1523-0901 was found to be a [[spectroscopic binary]] by a 2015 study.<ref name=Hansen2015/> The companion has a [[minimum mass]] about 11 times the [[Jupiter mass|mass of Jupiter]],<ref name=Schlaufman2018/> suggesting that it may be a [[brown dwarf]] or massive [[exoplanet]]. However, the discovery paper suggests that the companion's orbit may be nearly face-on, which would make the true mass much greater than the minimum mass, at about a quarter the [[Solar mass|mass of the Sun]].<ref name=Hansen2015/> Such an object would be a [[red dwarf]] star. The [[orbital inclination]] and thus true mass is not yet known with certainty. |
HE 1523-0901 was found to be a [[spectroscopic binary]] by a 2015 study.<ref name=Hansen2015/> The companion has a [[minimum mass]] about 11 times the [[Jupiter mass|mass of Jupiter]],<ref name=Schlaufman2018/> suggesting that it may be a [[brown dwarf]] or massive [[exoplanet]]. However, the discovery paper suggests that the companion's orbit may be nearly face-on, which would make the true mass much greater than the minimum mass, at about a quarter the [[Solar mass|mass of the Sun]].<ref name=Hansen2015/> Such an object would be a [[red dwarf]] star. The [[orbital inclination]] and thus true mass is not yet known with certainty. |
||
Planets around such metal-poor stars are rare; the only five known similar cases are [[HD 22781]], [[HD 111232]], [[HD 114762]], and [[HD 181720]].<ref>{{citation|arxiv=1902.04493|year=2019|doi=10.3390/geosciences9030105|last1=Adibekyan|first1=Vardan|title=Heavy Metal Rules. I. Exoplanet Incidence and Metallicity|journal=Geosciences|volume=9|issue=3|page=105|bibcode=2019Geosc...9..105A|s2cid=119089419|doi-access=free}}</ref> |
|||
HE 1523-0901 is the second metal-poor star that have companion star or planets after [[2MASS J18082002-5104378]] |
|||
{{OrbitboxPlanet begin |
{{OrbitboxPlanet begin |
||
| Line 71: | Line 66: | ||
| exoplanet = b |
| exoplanet = b |
||
| mass = {{val|11|4|1|p=≥}} |
| mass = {{val|11|4|1|p=≥}} |
||
| radius = |
| radius = |
||
| semimajor = |
| semimajor = |
||
| period = 303.05{{±|0.25}} |
| period = 303.05{{±|0.25}} |
||
| Line 82: | Line 77: | ||
*[[HD 140283]] |
*[[HD 140283]] |
||
*[[Sneden's Star]] |
*[[Sneden's Star]] |
||
*[[2MASS J18082002-5104378]] |
|||
==References== |
==References== |
||
| Line 117: | Line 111: | ||
== External links == |
== External links == |
||
*{{cite web|url=http://www.itwire.com.au/content/view/12098/1066/|title=Astronomers discover HE 1523-0901 star: Almost as old as universe|publisher=iTWire|access-date=2007-05-15|archive-url=https://web.archive.org/web/20070514034340/http://www.itwire.com.au/content/view/12098/1066/|archive-date=2007-05-14|url-status=dead}} |
*{{cite web|url=http://www.itwire.com.au/content/view/12098/1066/|title=Astronomers discover HE 1523-0901 star: Almost as old as universe|publisher=iTWire|access-date=2007-05-15|archive-url=https://web.archive.org/web/20070514034340/http://www.itwire.com.au/content/view/12098/1066/|archive-date=2007-05-14|url-status=dead}} |
||
*{{cite web|url=http://www.nbcnews.com/id/18612697|title=Ancient star nearly as old as the universe|date=11 May 2007 |publisher=NBC News|access-date=2007-05-14}} |
*{{cite web|url=http://www.nbcnews.com/id/18612697|archive-url=https://web.archive.org/web/20160305114949/http://www.nbcnews.com/id/18612697/|url-status=dead|archive-date=March 5, 2016|title=Ancient star nearly as old as the universe|date=11 May 2007 |publisher=NBC News|access-date=2007-05-14}} |
||
{{Sky|15|26|01.2|-|09|11|38|7500}} |
{{Sky|15|26|01.2|-|09|11|38|7500}} |
||
Latest revision as of 18:11, 3 August 2024
 Artist's impression of HE 1523-0901 | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Libra |
| Right ascension | 15h 26m 01.070s[1] |
| Declination | −09° 11′ 38.89″[1] |
| Apparent magnitude (V) | 11.129[2] |
| Characteristics | |
| Evolutionary stage | red giant branch[1] |
| Spectral type | CEMP[3] |
| B−V color index | +1.057[2] |
| Astrometry | |
| Radial velocity (Rv) | −162.48±0.34[1] km/s |
| Proper motion (μ) | RA: −22.685 mas/yr[1] Dec.: −28.204 mas/yr[1] |
| Parallax (π) | 0.3278 ± 0.0197 mas[1] |
| Distance | 9,900 ± 600 ly (3,100 ± 200 pc) |
| Details | |
| Mass | 0.80±0.01[4] M☉ |
| Radius | 27[1] R☉ |
| Luminosity | 730[1] L☉ |
| Surface gravity (log g) | 1.29±0.15[4] cgs |
| Temperature | 4,742±100[4] K |
| Metallicity [Fe/H] | −2.65±0.22[4] dex |
| Age | 13.2[5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HE 1523-0901 is the designation given to a red giant star in the Milky Way galaxy approximately 9,900 light-years from Earth. It is thought to be a second generation, Population II, or metal-poor, star ([Fe/H] = −2.95). The star was found in the sample of bright metal-poor halo stars from the Hamburg/ESO Survey by Anna Frebel and collaborators. The group's research was published in the May 10, 2007 issue of The Astrophysical Journal.[5]
Age
[edit]The star's age, as measured by ESO's Very Large Telescope, is 13.2 billion years. This makes it among the oldest stars[6] and nearly as old as the estimated age of the universe itself (13.8 billion years as measured by Planck). The measurement uncertainty in the age estimate is 0.7 to 2.7 billion years, depending upon the assumptions made to estimate the uncertainty, although the uncertainty in the relative age of this and other stars using the same method is smaller.[5] HE 1523-0901 is the first star whose age was determined using the decay of the radioactive elements uranium and thorium in tandem with measurements of several neutron capture elements.[7] It is believed to have formed directly from the remnants of the first-generation stars that reached the end of their longevity and exploded as supernovae early in the history of known matter.
Designation
[edit]The designation "HE 1523-0901" indicates that the star is part of the Hamburg/ESO Survey catalog. A list of astronomical catalogues can be used to find which catalog a star or other object is from based on its prefix. Most objects are listed in several catalogs and will often be known by several different designations.
Observation
[edit]HE 1523-0901 is approximately 0.8 solar masses, but the star has expanded until it is some 27 times as large, and has a total luminosity of 730 times that of the Sun. It can be viewed particularly well from the southern hemisphere with the use of a small telescope. It can also be observed from central European latitudes.
Spectroscopic companion
[edit]HE 1523-0901 was found to be a spectroscopic binary by a 2015 study.[8] The companion has a minimum mass about 11 times the mass of Jupiter,[9] suggesting that it may be a brown dwarf or massive exoplanet. However, the discovery paper suggests that the companion's orbit may be nearly face-on, which would make the true mass much greater than the minimum mass, at about a quarter the mass of the Sun.[8] Such an object would be a red dwarf star. The orbital inclination and thus true mass is not yet known with certainty.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥11+4 −1 MJ |
— | 303.05±0.25 | 0.163±0.010 | — | — |
See also
[edit]References
[edit]- ^ a b c d e f g h 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 Beers, Timothy C.; Flynn, Chris; Rossi, Silvia; Sommer-Larsen, Jesper; Wilhelm, Ronald; Marsteller, Brian; Lee, Young Sun; De Lee, Nathan; Krugler, Julie; Deliyannis, Constantine P.; Simmons, Andrew T.; Mills, Elisabeth; Zickgraf, Franz-Josef; Holmberg, Johan; Önehag, Anna; Eriksson, Anders; Terndrup, Donald M.; Salim, Samir; Andersen, Johannes; Nordström, Birgitta; Christlieb, Norbert; Frebel, Anna; Rhee, Jaehyon (2007). "Broadband UBVRCIC Photometry of Horizontal-Branch and Metal-poor Candidates from the HK and Hamburg/ESO Surveys. I.". The Astrophysical Journal Supplement Series. 168 (1): 128. arXiv:astro-ph/0610018. Bibcode:2007ApJS..168..128B. doi:10.1086/509324. S2CID 119500060.
- ^ Placco, Vinicius M.; Beers, Timothy C.; Santucci, Rafael M.; Chanamé, Julio; Sepúlveda, María Paz; Coronado, Johanna; Points, Sean D.; Kaleida, Catherine C.; Rossi, Silvia; Kordopatis, Georges; Lee, Young Sun; Matijevič, Gal; Frebel, Anna; Hansen, Terese T.; Holmbeck, Erika M.; Rasmussen, Kaitlin C.; Roederer, Ian U.; Sakari, Charli M.; Whitten, Devin D. (2018). "Spectroscopic Validation of Low-metallicity Stars from RAVE". The Astronomical Journal. 155 (6): 256. arXiv:1805.00608. Bibcode:2018AJ....155..256P. doi:10.3847/1538-3881/aac20c. S2CID 119460225.
- ^ a b c d Reggiani, Henrique; Ji, Alexander P.; Schlaufman, Kevin C.; Frebel, Anna; Necib, Lina; Nelson, Tyler; Hawkins, Keith; Galarza, Jhon Yana (2022). "The Chemical Composition of Extreme-velocity Stars". The Astronomical Journal. 163 (6): 252. arXiv:2203.16364. Bibcode:2022AJ....163..252R. doi:10.3847/1538-3881/ac62d9. S2CID 247793231.
- ^ a b c Frebel, A.; et al. (2007). "Discovery of HE 1523–0901, a Strongly r-Process-enhanced Metal-poor Star with Detected Uranium". The Astrophysical Journal. 660 (2): L117. arXiv:astro-ph/0703414. Bibcode:2007ApJ...660L.117F. doi:10.1086/518122. S2CID 17533424.
- ^ "Nearby Star Is A Galactic Fossil". Science Daily. May 11, 2007. Retrieved 2007-05-10.
- ^ "A galactic fossil: Star is found to be 13.2 billion years old". PhysOrg. May 10, 2007. Retrieved 2007-05-12.
- ^ a b Hansen, T. T.; Andersen, J.; Nordström, B.; Beers, T. C.; Yoon, J.; Buchhave, L. A. (2015), "The role of binaries in the enrichment of the early Galactic halo. I. r-process-enhanced metal-poor stars", Astronomy & Astrophysics, 583: A49, arXiv:1509.05344, Bibcode:2015A&A...583A..49H, doi:10.1051/0004-6361/201526812
- ^ a b Schlaufman, Kevin C.; Thompson, Ian B.; Casey, Andrew R. (2018), "An Ultra Metal-poor Star Near the Hydrogen-burning Limit", Astronomy & Astrophysics, 867 (2): 98, arXiv:1811.00549, Bibcode:2018ApJ...867...98S, doi:10.3847/1538-4357/aadd97
External links
[edit]- "Astronomers discover HE 1523-0901 star: Almost as old as universe". iTWire. Archived from the original on 2007-05-14. Retrieved 2007-05-15.
- "Ancient star nearly as old as the universe". NBC News. 11 May 2007. Archived from the original on March 5, 2016. Retrieved 2007-05-14.
