beta Trianguli

{{short description|Binary star in the constellation Triangulum}}

{{Starbox begin

| name = β Trianguli

}}

{{Starbox image

| image=

{{Location mark

|image=Triangulum constellation map.svg|alt=|float=center|width=280

|label=|position=right

|mark=Red circle.svg|mark_width=12|mark_link=β Trianguli

|x=517|y=319

}}

|caption=Location of β Trianguli (circled)

}}

{{Starbox observe

| epoch = J2000.0

| constell = Triangulum

| ra = {{RA|02|09|32.62712}}

| dec = {{DEC|+34|59|14.2694}}

| appmag_v = +3.00 (3.44 + 4.19)

}}

{{Starbox character

| class = A8III / A3III

| b-v = +0.21 / 0.07

| u-b = +0.11

| variable =

}}

{{Starbox astrometry

| radial_v = +9.9

| prop_mo_ra = 149.16

| prop_mo_dec = –39.10

| parallax = 23.169

| p_error = 0.434

| parallax_footnote =

| absmag_v = {{Val|-0.136}} (0.305 + 0.1055)

}}

{{Starbox orbit

| reference = {{citation | display-authors=1 | last1=Pourbaix | first1=D. | last2=Tokovinin | first2=A. A. | last3=Batten | first3=A. H. | last4=Fekel | first4=F. C. | last5=Hartkopf | first5=W. I. | last6=Levato | first6=H. | last7=Morrell | first7=N. I. | last8=Torres | first8=G. | last9=Udry | first9=S. | year=2004 | pages=727–732 | volume=424 | title=SB9: The Ninth Catalogue of Spectroscopic Binary Orbits | journal=Astronomy & Astrophysics | issue=2 | bibcode=2004A&A...424..727P | doi=10.1051/0004-6361:20041213 | postscript=. | arxiv=astro-ph/0406573 | s2cid=119387088 }}

| period_unitless = 31.3884 d

| eccentricity = 0.53

| axis_unitless = {{val|0.330|0.005}}

| periastron = 2432004.255 JD

| periarg = 318.4

| k1 = 33.3

| k2 = 69.2

}}

{{Starbox detail

| source =

| component1 = A

| mass = {{val|2.6|0.3}}

| radius = {{solar radius calculator|type=logLT|1.78|7683|decimals=2}}{{efn|name=radius1}}

| luminosity = {{val|60.3|15.6|12.4}}

| temperature = 7,683

| gravity = 3.70{{Cite journal | last1 = Gray | first1 = R. O. | last2 = Corbally | first2 = C. J. | last3 = Garrison | first3 = R. F. | last4 = McFadden | first4 = M. T. | last5 = Robinson | first5 = P. E. | title = Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I | doi = 10.1086/378365 | journal = The Astronomical Journal | volume = 126 | issue = 4 | pages = 2048 | year = 2003 |arxiv = astro-ph/0308182 |bibcode = 2003AJ....126.2048G | s2cid = 119417105 }}

| metal_fe =

| rotational_velocity = 70

| age_gyr = {{val|0.40|0.23|0.15}}

| component2 = B

| mass2 = {{val|2.25|0.05}}

| radius2 = {{solar radius calculator|type=logLT|1.50|8759|decimals=2}}{{efn|name=radius2}}

| luminosity2 = {{val|31.6|3.9|3.4}}

| temperature2 = 8,759

| age_gyr2 = {{val|0.45|0.12|0.09}}

}}

{{Starbox catalog

| names = β Trianguli, β Tri, Beta Tri, 4 Trianguli, HR 622, HD 13161, BD+34°381, FK5 75, HIP 10064, SAO 55306.

}}

{{Starbox reference

| Simbad = bet+Tri

}}

Beta Trianguli (Beta Tri, β Trianguli, β Tri) is the Bayer designation for a binary star system in the constellation Triangulum, located about 127 light years from Earth. Although it is only a third-magnitude star, it is the brightest star in the constellation Triangulum.

This is a double-lined spectroscopic binary star system with an orbital period of 31.39 days and an eccentricity of 0.53. The members are separated by a distance of {{val|0.33|ul=AU}}. The primary and secondary components have stellar classifications of A8III and A3III respectively, indicating that they evolved away from the main sequence and are now giant stars. Component A is 2.6 times more massive than the Sun, but expanded to {{solar radius calculator|type=logLT|1.78|7683|decimals=1}} the Sun's radius{{efn|name=radius1}} and irradiates 60 times more than the Sun. Component B is somewhat smaller and less luminous, being 2.25 times more massive, {{solar radius calculator|type=logLT|1.50|8759|decimals=2}} times larger{{efn|name=radius2}} and 30 times brighter than the Sun. The system has an age around 400 million years, less than 10% that of the Solar System. Beta Trianguli is among the least variable of the stars that were observed by the Hipparcos spacecraft, with a magnitude varying by only 0.0005.

Based on observations using the Spitzer Space Telescope, as reported in 2005, this system is emitting an excess of infrared radiation. This emission can be explained by a circumbinary ring of dust. The dust is emitting infrared radiation at a blackbody temperature of 100 K. It is thought to extend from 50 to 400 AU away from the stars.{{cite journal|author1=Kennedy, G. M. |author2=Wyatt, M. C. |author3=Sibthorpe, B. |author4=Phillips, N. M. |author5=Matthews, B. |author6=Greaves, J. S. |date=2012|title=Coplanar Circumbinary Debris Disks|journal=Monthly Notices of the Royal Astronomical Society|volume=426|issue=3|pages=2115–28|bibcode=2012MNRAS.426.2115K|doi=10.1111/j.1365-2966.2012.21865.x|doi-access=free |arxiv = 1208.1759 |s2cid=59408005 }}

Naming

In combination with Alpha Trianguli, these stars were called Al Mīzān, which is Arabic for "The Scale Beam".
In Chinese, {{lang|zh|天大將軍}} ({{lang|zh-Latn|Tiān Dà Jiāng Jūn}}), meaning Heaven's Great General, refers to an asterism consisting of β Trianguli, γ Andromedae, φ Persei, 51 Andromedae, 49 Andromedae, χ Andromedae, υ Andromedae, τ Andromedae, 56 Andromedae, γ Trianguli and δ Trianguli. Consequently, the Chinese name for β Trianguli itself is {{lang|zh|天大將軍九}} ({{lang|zh-Latn|Tiān Dà Jiāng Jūn jiǔ}}, {{langx|en|the Ninth Star of Heaven's Great General}}.).{{in lang|zh}} [http://aeea.nmns.edu.tw/2006/0607/ap060710.html AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 10 日] {{Webarchive|url=https://web.archive.org/web/20110716123113/http://aeea.nmns.edu.tw/2006/0607/ap060710.html |date=2011-07-16 }}

Notes

{{notelist|notes=

{{Efn|name=radius1|1=Calculated, using the Stefan-Boltzmann law and the star's effective temperature and luminosity, with respect to the solar nominal effective temperature of 5,772 K: $\sqrt{\biggl(\frac{5,772}{7,683}\biggr)^4 \cdot 10^{1.78}} = 4.38\ R_\odot.$ }}

{{Efn|name=radius2|1=Calculated, using the Stefan-Boltzmann law and the star's effective temperature and luminosity, with respect to the solar nominal effective temperature of 5,772 K: $\sqrt{\biggl(\frac{5,772}{8,759}\biggr)^4 \cdot 10^{1.50}} = 2.44\ R_\odot.$ }}

}}

References

{{Reflist|30em|refs=

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{{Citation |last=Groenewegen |first=M. A. T. |date=2023-01-01 |title=Orbital parallax of binary systems compared to Gaia DR3 and the parallax zero-point offset at bright magnitudes |arxiv=2210.14734 |journal=Astronomy and Astrophysics |volume=669 |pages=A4 |doi=10.1051/0004-6361/202244479 |bibcode=2023A&A...669A...4G|issn=0004-6361}} [https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A%2BA/669/A4&Name=02095%2B3459 Beta Trianguli's database entry].

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{{citation | title=bet Tri -- Spectroscopic binary | work=SIMBAD | publisher=Centre de Données astronomiques de Strasbourg | url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Beta+Trianguli | access-date=2011-12-12 }}

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}}

Category:A-type subgiants

Category:Spectroscopic binaries

beta Trianguli

Naming

See also

Notes

References