Gliese 514#Planetary system

{{Starbox begin

|name=Gliese 514

}}

{{Starbox observe

| epoch = J2000

| constell = Virgo

| ra = {{RA|13|29|59.78590}}

| dec = {{DEC|+10|22|37.7845}}

| appmag_v = 9.029

}}

{{Starbox character

| type = main-sequence star

| class = M0Ve{{citation|arxiv=2105.09014|year=2021|title=Astrometric radial velocities for nearby stars|doi=10.1051/0004-6361/202141344|last1=Lindegren|first1=Lennart|last2=Dravins|first2=Dainis|journal=Astronomy & Astrophysics|volume=652|pages=A45|bibcode=2021A&A...652A..45L|s2cid=234778154}}

| appmag_1_passband = J

| appmag_1 = 5.902{{±|0.018}}{{citation|arxiv=1705.08785|year=2017|title=Metallicity determination of M dwarfs|doi=10.1051/0004-6361/201730715|last1=Lindgren|first1=Sara|last2=Heiter|first2=Ulrike|journal=Astronomy & Astrophysics|volume=604|pages=A97|bibcode=2017A&A...604A..97L |s2cid=119216828}}

| appmag_2_passband = H

| appmag_2 = 5.300{{±|0.033}}

}}

{{Starbox astrometry

| radial_v = {{val|14.12|0.12}}

| prop_mo_ra = {{val|1127.341|fmt=commas}}

| prop_mo_dec = {{val|−1073.888|fmt=commas}}

| pm_footnote =

| parallax = 131.1013

| p_error = 0.0270

| parallax_footnote =

| absmag_v = +9.63{{cite XHIP|65859|mode=cs2}}

}}

{{Starbox detail

| source =

| mass = 0.562

| radius = 0.611{{±|0.043}}{{citation|arxiv=astro-ph/0602105|year=2006|title=First Results from the CHARA Array. IV. The Interferometric Radii of Low-Mass Stars|doi=10.1086/503318|last1=Berger|first1=D. H.|last2=Gies|first2=D. R.|last3=McAlister|first3=H. A.|last4=Brummelaar|first4=T. A. ten|last5=Henry|first5=T. J.|last6=Sturmann|first6=J.|last7=Sturmann|first7=L.|last8=Turner|first8=N. H.|last9=Ridgway|first9=S. T.|last10=Aufdenberg|first10=J. P.|last11=Merand|first11=A.|journal=The Astrophysical Journal|volume=644|issue=1|pages=475–483|bibcode=2006ApJ...644..475B|s2cid=14966363}}

| temperature = 2,901{{citation|arxiv=2002.05762|year=2020|title=Understanding the physical properties of young M dwarfs: NIR spectroscopic studies|doi=10.1093/mnras/staa427|last1=Ghosh|first1=Samrat|last2=Ghosh|first2=Supriyo|last3=Das|first3=Ramkrishna|last4=Mondal|first4=Soumen|last5=Khata|first5=Dhrimadri|journal=Monthly Notices of the Royal Astronomical Society|volume=493|issue=3|pages=4533–4550|doi-access=free |bibcode=2020MNRAS.493.4533K }} - 3,727

| luminosity_bolometric = 0.043

| gravity = 4.78

| metal_fe = {{val|−0.07|0.07}}

| rotation = 28.0{{±|2.9}} days

| rotational_velocity = 2.00

| age_gyr = 8.25{{citation |bibcode=2020A&A...644A..68M |title=HADES RV programme with HARPS-N at TNG. XII. The abundance signature of M dwarf stars with planets |last1=Maldonado |first1=J. |last2=Micela |first2=G. |last3=Baratella |first3=M. |last4=d'Orazi |first4=V. |last5=Affer |first5=L. |last6=Biazzo |first6=K. |last7=Lanza |first7=A. F. |last8=Maggio |first8=A. |last9=González Hernández |first9=J. I. |last10=Perger |first10=M. |last11=Pinamonti |first11=M. |last12=Scandariato |first12=G. |last13=Sozzetti |first13=A. |last14=Locci |first14=D. |last15=Di Maio |first15=C. |last16=Bignamini |first16=A. |last17=Claudi |first17=R. |last18=Molinari |first18=E. |last19=Rebolo |first19=R. |last20=Ribas |first20=I. |last21=Toledo-Padrón |first21=B. |last22=Covino |first22=E. |last23=Desidera |first23=S. |last24=Herrero |first24=E. |last25=Morales |first25=J. C. |last26=Suárez-Mascareño |first26=A. |last27=Pagano |first27=I. |last28=Petralia |first28=A. |last29=Piotto |first29=G. |last30=Poretti |first30=E. |journal=Astronomy and Astrophysics |year=2020 |volume=644 |pages=A68 |doi=10.1051/0004-6361/202039478 |arxiv=2010.14867 |s2cid=225094682 }}

}}

{{Starbox catalog

| names = {{odlist|BD=+11 2576|2MASS = J13295979+1022376|Ross=490|TYC=895-317-1|HIP=65859|LTT=13925}}, Gaia EDR3 3738099879558957952{{cite simbad|title=BD+11 2576|access-date=2022-04-17 |mode=cs2 }}

}}

{{Starbox reference

| Simbad = BD%2B11+2576

| NSTED = GJ-514

}}

Gliese 514, also known as BD+11 2576 or HIP 65859, is an M-type main-sequence star, in the constellation Virgo 24.88 light-years away from the Solar System.

Gliese 514's metallicity Fe/H index is largely unknown, with median values from -0.4 to +0.18 reported in the literature. This discrepancy is due to peculiarities of the stellar spectrum of Gliese 514.{{cn|date=March 2025}} The spectrum peculiarities also affect the accuracy of the star's temperature measurement,{{citation|arxiv=2102.08836|year=2021|title=Comparative high-resolution spectroscopy of M dwarfs: Exploring non-LTE effects|doi=10.1051/0004-6361/202039747|last1=Olander|first1=T.|last2=Heiter|first2=U.|last3=Kochukhov|first3=O.|journal=Astronomy & Astrophysics|volume=649|pages=A103|bibcode=2021A&A...649A.103O|s2cid=231942628}} with reported values as low as 2901 K. The spectrum of Gliese 514 shows emission lines, but the star itself has a low starspot activity.{{citation |bibcode=2007A&A...467..259R |title=The narrowest M-dwarf line profiles and the rotation-activity connection at very slow rotation |last1=Reiners |first1=A. |journal=Astronomy and Astrophysics |year=2007 |volume=467 |issue=1 |page=259 |doi=10.1051/0004-6361:20066991 |arxiv=astro-ph/0702634 |s2cid=8672566 }}

Multiplicity surveys did not detect any stellar companions as of 2020.{{citation|arxiv=2001.05988|year=2020|title=Robo-AO M-dwarf Multiplicity Survey: Catalog|doi=10.3847/1538-3881/ab6ef1|last1=Lamman|first1=Claire|last2=Baranec|first2=Christoph|last3=Berta-Thompson|first3=Zachory K.|last4=Law|first4=Nicholas M.|last5=Schonhut-Stasik|first5=Jessica|last6=Ziegler|first6=Carl|last7=Salama|first7=Maïssa|last8=Jensen-Clem|first8=Rebecca|last9=Duev|first9=Dmitry A.|last10=Riddle|first10=Reed|last11=Kulkarni|first11=Shrinivas R.|last12=Winters|first12=Jennifer G.|last13=Irwin|first13=Jonathan M.|journal=The Astronomical Journal|volume=159|issue=4|page=139|bibcode=2020AJ....159..139L|s2cid=210718832 |doi-access=free }}

The Sun is currently calculated to be passing through the tidal tail of Gliese 514's Oort cloud. Thus, future interstellar objects passing through the Solar System may originate from Gliese 514.{{citation |arxiv=2011.08257 |doi=10.1051/0004-6361/202038888 |title=Oort cloud Ecology |year=2021 |last1=Portegies Zwart |first1=S. |journal=Astronomy & Astrophysics |volume=647 |pages=A136 |s2cid=226976082 }}

Planetary system

The existence of a planet on a 15-day orbit around Gliese 514 was first suspected in 2019.{{cite arXiv|last1=Barnes|first1=J. R.|last2=Kiraga|first2=M.|last3=Diaz|first3=M.|last4=Berdiñas|first4=Z.|last5=Jenkins|first5=J. S.|last6=Keiser|first6=S.|last7=Thompson|first7=I.|last8=Crane|first8=J. D.|last9=Shectman|first9=S. A.|display-authors=1|date=2019-06-11|title=Frequency of planets orbiting M dwarfs in the Solar neighbourhood|class=astro-ph.EP|eprint=1906.04644|language=en}} However, that planet was not confirmed. Instead, in 2022, one Super-Earth planet, named Gliese 514 b, was discovered on an eccentric 140-day orbit by the radial velocity method. The planetary orbit partially lies within the habitable zone of the parent star with planetary equilibrium temperature, averaged along orbit, equal to {{val|202|11|ul=K}}.{{citation|arxiv=2204.06376|year=2022|title=A quarter century of spectroscopic monitoring of the nearby M dwarf Gl 514|last1=Damasso|first1=M.|last2=Perger|first2=M.|last3=Almenara|first3=J. M.|last4=Nardiello|first4=D.|last5=Pérez-Torres|first5=M.|last6=Sozzetti|first6=A.|last7=Hara|first7=N. C.|last8=Quirrenbach|first8=A.|last9=Bonfils|first9=X.|last10=Zapatero Osorio|first10=M. R.|last11=Astudillo-Defru|first11=N.|last12=González Hernández|first12=J. I.|last13=Suárez Mascareño|first13=A.|last14=Amado|first14=P. J.|last15=Forveille|first15=T.|last16=Lillo-Box|first16=J.|last17=Alibert|first17=Y.|last18=Caballero|first18=J. A.|last19=Cifuentes|first19=C.|last20=Delfosse|first20=X.|last21=Figueira|first21=P.|last22=Galadí-Enríquez|first22=D.|last23=Hatzes|first23=A. P.|last24=Henning|first24=Th.|last25=Kaminski|first25=A.|last26=Mayor|first26=M.|last27=Murgas|first27=F.|last28=Montes|first28=D.|last29=Pinamonti|first29=M.|last30=Reiners|first30=A.|journal=Astronomy & Astrophysics |volume=666 |pages=A187 |doi=10.1051/0004-6361/202243522 |s2cid=248157318 |display-authors=1}}

The infrared excess of the star also indicates the possible presence of a debris disk in the system, albeit at a low signal to noise ratio.{{citation|arxiv=2004.12597|year=2020|title=Herschel Observations of Disks around Late-type Stars|doi=10.1088/1538-3873/ab895f|last1=Tanner|first1=Angelle|last2=Plavchan|first2=Peter|last3=Bryden|first3=Geoff|last4=Kennedy|first4=Grant|last5=Matrá|first5=Luca|last6=Cronin-Coltsmann|first6=Patrick|last7=Lowrance|first7=Patrick|last8=Henry|first8=Todd|last9=Riaz|first9=Basmah|last10=Gizis|first10=John E.|last11=Riedel|first11=Adric|last12=Choquet|first12=Elodie|journal=Publications of the Astronomical Society of the Pacific|volume=132|issue=1014|page=084401|bibcode=2020PASP..132h4401T|s2cid=216553868}}

{{OrbitboxPlanet begin

| name = Gliese 514

| table_ref =

}}

{{OrbitboxPlanet

| exoplanet = b

| mass_earth = >5.2{{±|0.9}}

| radius =

| semimajor = 0.422{{±|0.014|0.015}}

| period = 140.43{{±|0.41}}

| eccentricity = 0.45{{±|0.15|0.14}}

| inclination =