Mu Pegasi

{{Starbox image

| image =

{{Location mark

| image=Pegasus IAU.svg

| float=center | width=250 | position=right

| mark=Red circle.svg | mark_width=10 | mark_link=ι Exa

| x%=44.5 | y%=37.8

}}

| caption=Location of μ Pegasi (circled)

}}

{{Starbox observe

| epoch = J2000.0

| ra = {{RA|22|50|00.19307}}

| dec = {{DEC|+24|36|05.6926}}

| appmag_v = 3.514

| constell = Pegasus

}}

{{Starbox character

| type = Yellow giant

| class = G8 III

| b-v = +0.932

| u-b = +0.674

| variable =

}}

{{Starbox astrometry

| radial_v = {{nowrap|+13.54 ± 0.20}}

| prop_mo_ra = +145.240

| prop_mo_dec = {{val|-42.396}}

| pm_footnote =

| parallax = 28.934

| p_error = 0.189

| parallax_footnote =

| absmag_v = +0.432

}}

{{Starbox detail

| mass = {{val|2.59|0.05}}

| radius = {{val|9.32|0.47}}

| luminosity = {{val|46.9|0.6}}

| temperature = {{Val|4961|40|fmt=commas}}

| gravity = {{val|2.85|0.03}}

| metal_fe = {{val|-0.03|0.02}}

| rotational_velocity = {{val|0.95|0.45}}

| rotation =

| age_myr = {{val|520|30}}

}}

{{Starbox catalog

| names = {{odlist | name=Sadalbari | B=Mu Peg, μ Peg | F=48 Peg | BD=+23 4615 | FK5=862 | GJ=4298 | HD=216131 | HIP=112748 | HR=8684 | SAO=90816 }}

}}

{{Starbox reference

|Simbad=mu+Peg

}}

Mu Pegasi or μ Pegasi, formally named Sadalbari ({{IPAc-en|,|s|æ|d|@l|'|b|ɛər|i}}), is a star in the northern constellation of Pegasus. The apparent visual magnitude of this star is 3.5, which is bright enough to be seen with the naked eye even on a moonlit night. Based upon parallax measurements taken by the Gaia spacecraft, it is approximately {{Convert|113|ly|pc|abbr=off|lk=on}} from the Sun.

Nomenclature

μ Pegasi (Latinised to Mu Pegasi) is the star's Bayer designation.

It bore the traditional name Sadalbari, which derives from {{langx|ar|سعد بارع}} saʿd al-bāriʿ, the “auspicious star of the splendid one.”{{cite book |author = Allen, Richard Hinckley |author-link = Richard Hinckley Allen |year = 1963 |orig-year = 1899 |title = Star Names: Their Lore and Meaning |edition = rep. |publisher = Dover Publications Inc. |location = New York, NY |url = https://archive.org/details/starnamestheirlo00alle/page/328 |isbn = 0-486-21079-0 |pages = [https://archive.org/details/starnamestheirlo00alle/page/328 328–29] |url-access = registration}} In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN){{citation | url=https://www.iau.org/science/scientific_bodies/working_groups/280/ | title=IAU Working Group on Star Names (WGSN) | publisher=International Astronomical Union | access-date=22 May 2016 | postscript=.}} to catalogue and standardize proper names for stars. The WGSN approved the name Sadalbari for this star on 21 August 2016 and it is now so included in the List of IAU-approved Star Names.

In Chinese, {{lang|zh|離宮}} ({{lang|zh-Latn|Lì Gōng}}), meaning Resting Palace, refers to an asterism consisting of Mu Pegasi, Lambda Pegasi, Omicron Pegasi, Eta Pegasi, Tau Pegasi and Nu Pegasi.{{in lang|zh}} 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, {{ISBN|978-986-7332-25-7}}. Consequently, the Chinese name for Mu Pegasi itself is {{lang|zh|離宮二}} ({{lang|zh-Latn|Lì Gōng èr}}, "the Second Star of Resting Palace").{{in lang|zh}} [http://www.lcsd.gov.hk/CE/Museum/Space/Research/StarName/c_research_chinengstars_ala_alz.htm 香港太空館 - 研究資源 - 亮星中英對照表] {{webarchive|url=https://web.archive.org/web/20081025110153/http://www.lcsd.gov.hk/CE/Museum/Space/Research/StarName/c_research_chinengstars_ala_alz.htm |date=2008-10-25}}, Hong Kong Space Museum. Accessed on line November 23, 2010.

Properties

The spectrum of this star matches a stellar classification of G8 III. The luminosity class of 'III' means that it has exhausted the hydrogen fuel at its core and evolved into a giant star. It is 520 million years old and 2.6 times more massive than the Sun, but has expanded to nine times the Sun's radius. The effective temperature of the outer atmosphere is about 4,961 K, which is cooler than the Sun and gives it the yellow hue of a G-type star. The abundance of elements other than hydrogen and helium, what astronomers term the metallicity, is a bit smaller than the abundance in the Sun.

References

{{reflist|refs=

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{{Citation |last1=Soubiran |first1=C. |last2=Creevey |first2=O. L. |last3=Lagarde |first3=N. |last4=Brouillet |first4=N. |last5=Jofré |first5=P. |last6=Casamiquela |first6=L. |last7=Heiter |first7=U. |last8=Aguilera-Gómez |first8=C. |last9=Vitali |first9=S. |last10=Worley |first10=C. |last11=de Brito Silva |first11=D. |date=2024-02-01 |title=Gaia FGK benchmark stars: Fundamental Teff and log g of the third version |bibcode=2024A&A...682A.145S |journal=Astronomy and Astrophysics |volume=682 |pages=A145 |doi=10.1051/0004-6361/202347136 |arxiv=2310.11302 |issn=0004-6361}} [https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A%2BA/682/A145&HIP=HIP112748 Mu Pegasi's database entry] at VizieR.

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{{citation | title=48 Peg -- High proper-motion Star | work=SIMBAD | publisher=Centre de Données astronomiques de Strasbourg | url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD+216131 | access-date=2012-01-28}}

{{citation | first1=James B. | last1=Kaler | title=SADALBARI (Lambda and Mu Pegasi) | work=Stars | publisher=University of Illinois | url=http://stars.astro.illinois.edu/sow/sadalbari.html | access-date=2012-01-28}}

{{citation | title=The Colour of Stars | date=December 21, 2004 | work=Australia Telescope, Outreach and Education | publisher=Commonwealth Scientific and Industrial Research Organisation | url=http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html | access-date=2012-01-16 | archive-url=https://web.archive.org/web/20120318151427/http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html | archive-date=March 18, 2012 | url-status=dead}}

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{{cite web | url=https://www.iau.org/public/themes/naming_stars/ | title=Naming Stars |publisher=IAU.org |access-date=16 December 2017}}

}}

Category:G-type giants

Category:Pegasus (constellation)

Pegasi, Mu

Category:Durchmusterung objects