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{{Short description|Star in constellation Canes Venatici}}
{{Short description|Star in constellation Canes Venatici}}
{{Starbox begin
{{Starbox begin}}
| name = Gliese 806
}}
{{Starbox observe
{{Starbox observe
|epoch=[[J2000]]
| epoch = [[J2000]]
| constell = [[Canes Venatici]]
| constell = [[Canes Venatici]]
| ra = {{RA|13|29|24.10}}
| ra = {{RA|13|29|24.102}}<ref name=GaiaDR2/>
| dec = {{DEC|+46|11|11.37}}
| dec = {{DEC|+46|11|11.36}}<ref name=GaiaDR2/>
| appmag_v = +10.26
| appmag_v = +10.26<ref name=Jenkins_et_al_2006/>
}}
}}
{{Starbox character
{{Starbox character
| class = M1V
| type =
| class = M1V<ref name=Alonso-Floriano_et_al_2015/>
| appmag_1_passband = J
| appmag_1 = 7.05<ref name=Jenkins_et_al_2006/>
| appmag_2_passband = H
| appmag_2 = 6.51<ref name=Jenkins_et_al_2006/>
| appmag_3_passband = K
| appmag_3 = 6.26<ref name=Jenkins_et_al_2006/>
| b-v =
| variable =
}}
}}
{{Starbox astrometry
{{Starbox astrometry
| radial_v = −65.55{{±|0.62}}<ref name=Houdebine2010/>
| dist_ly = 43.22
| dist_pc = 13.26
| prop_mo_ra = −42.466
| prop_mo_dec = 389.084
| pm_footnote = <ref name=GaiaDR2/>
| parallax = 74.8051
| p_error = 0.0257
| parallax_footnote = <ref name=GaiaDR2/>
| absmag_v = 10.243<ref name=Houdebine2010/>
}}
}}
{{Starbox detail
{{Starbox detail
| mass = {{val|0.506|0.021|u=Solar mass}}<ref name=Jenkins_et_al_2006/><br>0.47{{±|0.05}}<ref name=Maldonado_et_al_2017/>
| mass = 0.56
| radius = {{val|0.619|0.030|u=Solar radius}}<ref name=Houdebine2010/><br>0.47{{±|0.05}}<ref name=Maldonado_et_al_2017/>
| radius = 0.48
| luminosity = 0.041
| luminosity = {{val|0.033|0.008|0.007}}<ref name=Maldonado_et_al_2017/>
| temperature = {{val|3740}}
| temperature = {{val|3493|50|fmt=commas}}<ref name=Houdebine2010/>
| gravity = 4.79{{±|0.04}}<ref name=Maldonado_et_al_2017/>
| metal_fe = {{val|−0.34|u=dex}}<ref name=Jenkins_et_al_2006/><br>−0.09{{±|0.09}}<ref name=Maldonado_et_al_2017/>
| age_gyr =
| rotation = {{val|49.5|3.5|u=days}}<ref name=Suárez_Mascareño_et_al_2018/>
| rotational_velocity = 0.85<ref name=Houdebine2010/>
}}
}}
{{Starbox catalog
{{Starbox catalog
| names = HIP 66625, GJ 521, TYC 3463-00063-1, BD+46 1889, 2MASS J13392410+4611114
| names = {{odlist | HIP=66625 | GJ=521 | LTT=13979 | SAO=44697 | TYC=3463-00063-1 | BD=+46 1889 | 2MASS=J13392410+4611114 | WDS=13394+4611 }}<ref name=SIMBAD/>
}}
}}
{{Starbox reference
{{Starbox reference
| Simbad = GJ+521
| Simbad = GJ+521
}}
}}
{{Starbox end}}
{{Starbox end}}


'''Gliese 521''' is a [[double star]] in the northern [[constellation]] of [[Canes Venatici]]. The primary is suspected to host a [[substellar]] companion yet unconfirmed. The system is located at a distance of 43.6&nbsp;[[light-year]]s from the [[Sun]] based on [[stellar parallax|parallax]] measurements, but is drawing closer with a [[radial velocity]] of −65.6&nbsp;km/s.<ref name=Houdebine2010/> It is predicted to come as close as {{convert|4.814|pc|ly|disp=out|abbr=off}} from the Sun in 176,900&nbsp;years.<ref name=Bailer-Jones2018/> This star is too faint to be visible to the naked eye, having an [[apparent visual magnitude]] of +10.26<ref name=Jenkins_et_al_2006/> and an [[absolute magnitude]] of 10.24.<ref name=Houdebine2010/>
'''Gliese 521''' is a [[red dwarf star]] in the constellation of [[Canes Venatici]], located roughly 43 [[light year]]s from the [[Sun]]. The star is suspected to host a [[substellar]] companion yet unconfirmed.

The primary is an [[M-type main-sequence star]] with a [[stellar classification]] of M1V.<ref name=Alonso-Floriano_et_al_2015/> It is only about half the size and mass of the Sun. The star is rotating slowly with a [[projected rotational velocity]] of 0.85&nbsp;km/s<ref name=Houdebine2010/> and a [[rotation period]] of roughly 49.5&nbsp;days.<ref name=Suárez_Mascareño_et_al_2018/> The star has a lower [[metallicity|metal]]-content compared to the Sun. It is radiating just 3%<ref name=Maldonado_et_al_2017/> of the luminosity of the Sun from its [[photosphere]] at an [[effective temperature]] of 3,493&nbsp;K.<ref name=Houdebine2010/>

A faint stellar companion was announced by E. Jódar and associates in 2013. The companion has an [[angular separation]] of {{val|521|ul=mas}} along a [[position angle]] of 352.1°{{±|1.4}}° from the primary. This is equivalent to a [[projected separation]] of {{val|7.24|0.14|ul=AU}}.<ref name=Jódar_et_al_2013/>


== A planetary companion? ==
== A planetary companion? ==


According to Marcy & Benitz (1989)<ref name="Marcy & Benitz">{{cite journal| doi=10.1086/167812| author=Marcy & Benitz| last2=Benitz| first2=Karsten J.| title=A search for substellar companions to low-mass stars| journal=Astrophysical Journal, Part 1| volume=344|issue=1|pages=441–453 |year=1989|bibcode=1989ApJ...344..441M}}</ref> detected a possible periodicity of 510 [[day]]s, inferring possible presence of a massive planetary object with minimum mass of 12 times that of [[Jupiter]] in highly eccentric orbit (e=0.6). So far the planet has not been confirmed.
According to Marcy & Benitz (1989)<ref name="Marcy & Benitz"/> detected a possible periodicity of 510 [[day]]s, inferring possible presence of a massive planetary object with minimum mass of 12 times that of [[Jupiter]] in highly eccentric orbit (e=0.6). So far the planet has not been confirmed. A radial velocity study of the star during the period 2013–2017 initially found a promising signal, but this disappeared when additional data was collected and was instead attributed to magnetic activity.<ref name=Gonzalez_Alvarez_2018/>


{{OrbitboxPlanet begin
{{OrbitboxPlanet begin
| table_ref=<ref name="Marcy & Benitz" />
| table_ref=<ref name="Marcy & Benitz" />
| period_unit=day
| period_unit=day
}}
}}
{{OrbitboxPlanet hypothetical
{{OrbitboxPlanet hypothetical
| exoplanet = b
| exoplanet = b
| mass = ≥12
| mass = ≥12
| period = 510
| period = 510
| semimajor = 1.038
| semimajor = 1.038
| eccentricity = 0.6
| eccentricity = 0.6
}}
}}
{{Orbitbox end}}
{{Orbitbox end}}
Line 55: Line 77:


==References==
==References==
{{reflist}}
{{reflist|refs=

<ref name=GaiaDR2>{{Cite Gaia DR2|1503625448550796032}}</ref>

<ref name=SIMBAD>{{cite simbad
| title=BD+46 1889 | access-date=2021-11-21 }}</ref>

<ref name=Alonso-Floriano_et_al_2015>{{cite journal
| title=CARMENES input catalogue of M dwarfs. I. Low-resolution spectroscopy with CAFOS
| last1=Alonso-Floriano | first1=F. J. | last2=Morales | first2=J. C.
| last3=Caballero | first3=J. A. | last4=Montes | first4=D.
| last5=Klutsch | first5=A. | last6=Mundt | first6=R.
| last7=Cortés-Contreras | first7=M. | last8=Ribas | first8=I.
| last9=Reiners | first9=A. | last10=Amado | first10=P. J.
| last11=Quirrenbach | first11=A. | last12=Jeffers | first12=S. V.
| display-authors=1 | journal=Astronomy & Astrophysics
| volume=577 | id=A128 | pages=19 | date=May 2015
| doi=10.1051/0004-6361/201525803 | arxiv=1502.07580
| bibcode=2015A&A...577A.128A }}</ref>

<ref name="Marcy & Benitz">{{cite journal
| title=A search for substellar companions to low-mass stars
| last1=Marcy | first1=Geoffrey W. | last2=Benitz | first2=Karsten J.
| journal=Astrophysical Journal, Part 1
| volume=344 | issue=1 | pages=441–453 | date=September 1989
| doi=10.1086/167812 | bibcode=1989ApJ...344..441M }}</ref>

<ref name=Houdebine2010>{{cite journal
| title=Observation and modelling of main-sequence star chromospheres - XIV. Rotation of dM1 stars
| last=Houdebine | first=E. R.
| journal=Monthly Notices of the Royal Astronomical Society
| volume=407 | issue=3 | pages=1657–1673 | date=September 2010
| doi=10.1111/j.1365-2966.2010.16827.x | bibcode=2010MNRAS.407.1657H }}</ref>

<ref name=Bailer-Jones2018>{{cite journal
| title=The completeness-corrected rate of stellar encounters with the Sun from the first Gaia data release
| last=Bailer-Jones | first=C. A. L.
| journal=Astronomy & Astrophysics
| volume=609 | id=A8 | pages=16 | date=January 2018
| arxiv=1708.08595 | bibcode=2018A&A...609A...8B
| doi=10.1051/0004-6361/201731453 | s2cid=119462489 }}</ref>

<ref name=Suárez_Mascareño_et_al_2018>{{cite journal
| title=HADES RV programme with HARPS-N at TNG. VII. Rotation and activity of M-dwarfs from time-series high-resolution spectroscopy of chromospheric indicators
| display-authors=1 | last1=Suárez Mascareño | first1=A.
| last2=Rebolo | first2=R. | last3=González Hernández | first3=J. I.
| last4=Toledo-Padrón | first4=B. | last5=Perger | first5=M.
| last6=Ribas | first6=I. | last7=Affer | first7=L.
| last8=Micela | first8=G. | last9=Damasso | first9=M.
| last10=Maldonado | first10=J. | last11=González-Alvarez | first11=E.
| last12=Leto | first12=G. | last13=Pagano | first13=I.
| last14=Scandariato | first14=G. | last15=Sozzetti | first15=A.
| last16=Lanza | first16=A. F. | last17=Malavolta | first17=L.
| last18=Claudi | first18=R. | last19=Cosentino | first19=R.
| last20=Desidera | first20=S. | last21=Giacobbe | first21=P.
| last22=Maggio | first22=A. | last23=Rainer | first23=M.
| last24=Esposito | first24=M. | last25=Benatti | first25=S.
| last26=Pedani | first26=M. | last27=Morales | first27=J. C.
| last28=Herrero | first28=E. | last29=Lafarga | first29=M.
| last30=Rosich | first30=A. | last31=Pinamonti | first31=M.
| journal=Astronomy & Astrophysics
| volume=612 | id=A89 | pages=17 | date=April 2018
| doi=10.1051/0004-6361/201732143 | arxiv=1712.07375
| bibcode=2018A&A...612A..89S }}</ref>

<ref name=Jenkins_et_al_2006>{{Cite journal
| title=Rotational Velocities for M Dwarfs
| display-authors=1 | last1=Jenkins | first1=J. S.
| last2=Ramsey | first2=L. W. | last3=Jones | first3=H. R. A.
| last4=Pavlenko | first4=Y. | last5=Gallardo | first5=J.
| last6=Barnes | first6=J. R. | last7=Pinfield | first7=D. J.
| last8=Laughlin | first8=G. | last9=Holden | first9=B.
| last10=Teske | first10=J. K. | last11=Shectman | first11=S. A.
| last12=Crane | first12=J. D. | last13=Thompson | first13=I.
| last14=Keiser | first14=S. | last15=Jenkins | first15=J. S.
| last16=Berdiñas | first16=Z. | last17=Diaz | first17=M.
| last18=Kiraga | first18=M. | last19=Barnes | first19=J. R.
| journal=The Astrophysical Journal
| volume=704 | issue=2 | pages=975 | year=2009
| bibcode=2009ApJ...704..975J | arxiv=0908.4092
| doi=10.1088/0004-637X/704/2/975 | s2cid=119203469 }}</ref>

<ref name=Jódar_et_al_2013>{{cite journal
| title=New companions to nearby low-mass stars
| last1=Jódar | first1=Esther | last2=Pérez-Garrido | first2=Antonio
| last3=Díaz-Sánchez | first3=Anastasio | last4=Villó | first4=Isidro
| last5=Rebolo | first5=Rafael | last6=Pérez-Prieto | first6=Jorge A.
| display-authors=1 | journal=Monthly Notices of the Royal Astronomical Society
| volume=429 | issue=1 | pages=859-867 | date=February 2013
| doi=10.1093/mnras/sts382 | bibcode=2013MNRAS.429..859J }}</ref>

<ref name=Maldonado_et_al_2017>{{cite journal
| title=HADES RV Programme with HARPS-N at TNG . III. Flux-flux and activity-rotation relationships of early-M dwarfs
| display-authors=1 | last1=Maldonado | first1=J.
| last2=Scandariato | first2=G. | last3=Stelzer | first3=B.
| last4=Biazzo | first4=K. | last5=Lanza | first5=A. F.
| last6=Maggio | first6=A. | last7=Micela | first7=G.
| last8=González-Álvarez | first8=E. | last9=Affer | first9=L.
| last10=Claudi | first10=R. U. | last11=Cosentino | first11=R.
| last12=Damasso | first12=M. | last13=Desidera | first13=S.
| last14=González Hernández | first14=J. I. | last15=Gratton | first15=R.
| last16=Leto | first16=G. | last17=Messina | first17=S.
| last18=Molinari | first18=E. | last19=Pagano | first19=I.
| last20=Perger | first20=M. | last21=Piotto | first21=G.
| last22=Rebolo | first22=R. | last23=Ribas | first23=I.
| last24=Sozzetti | first24=A. | last25=Suárez Mascareño
| first25=A. | last26=Zanmar Sanchez | first26=R.
| journal=Astronomy & Astrophysics
| volume=598 | id=A27 | pages=19 | date=February 2017
| doi=10.1051/0004-6361/201629223 | arxiv=1610.05906
| bibcode=2017A&A...598A..27M }}</ref>

<ref name=Gonzalez_Alvarez_2018>{{cite book
| title=Planets around low-mass stars and stellar activity effects
| last=Gonzalez Alvarez | first=Ester | year=2018
| work=Doctoral Thesis
| publisher=Università degli Studi di Palermo
| url=http://hdl.handle.net/10447/265375
| access-date=2021-11-21 }}</ref>

}}


{{Stars of Canes Venatici}}
{{Stars of Canes Venatici}}


{{DEFAULTSORT:Gliese 521}}
{{DEFAULTSORT:Gliese 521}}
[[Category:Canes Venatici]]
[[Category:M-type main-sequence stars]]
[[Category:M-type main-sequence stars]]
[[Category:Hypothetical planetary systems]]
[[Category:Hypothetical planetary systems]]
[[Category:Double stars]]
[[Category:Canes Venatici]]
[[Category:Durchmusterung objects]]
[[Category:Gliese and GJ objects|0521]]
[[Category:Gliese and GJ objects|0521]]
[[Category:Hipparcos objects|066625]]
[[Category:Hipparcos objects|066625]]
[[Category:Durchmusterung objects]]


{{Extrasolar-planet-stub}}
{{reddwarf-star-stub}}

Revision as of 22:02, 21 November 2021

Gliese 521
Observation data
Epoch J2000      Equinox J2000
Constellation Canes Venatici
Right ascension 13h 29m 24.102s[1]
Declination +46° 11′ 11.36″[1]
Apparent magnitude (V) +10.26[2]
Characteristics
Spectral type M1V[3]
Apparent magnitude (J) 7.05[2]
Apparent magnitude (H) 6.51[2]
Apparent magnitude (K) 6.26[2]
Astrometry
Radial velocity (Rv)−65.55±0.62[4] km/s
Proper motion (μ) RA: −42.466 mas/yr[1]
Dec.: 389.084 mas/yr[1]
Parallax (π)74.8051 ± 0.0257 mas[1]
Distance43.60 ± 0.01 ly
(13.368 ± 0.005 pc)
Absolute magnitude (MV)10.243[4]
Details
Mass0.506±0.021 M☉[2]
0.47±0.05[5] M☉
Radius0.619±0.030 R☉[4]
0.47±0.05[5] R☉
Luminosity0.033+0.008
−0.007[5] L☉
Surface gravity (log g)4.79±0.04[5] cgs
Temperature3,493±50[4] K
Metallicity [Fe/H]−0.34 dex[2]
−0.09±0.09[5] dex
Rotation49.5±3.5 d[6]
Rotational velocity (v sin i)0.85[4] km/s
Other designations
BD+46 1889, GJ 521, HIP 66625, SAO 44697, WDS 13394+4611, LTT 13979, TYC 3463-00063-1, 2MASS J13392410+4611114[7]
Database references
SIMBADdata

Gliese 521 is a double star in the northern constellation of Canes Venatici. The primary is suspected to host a substellar companion yet unconfirmed. The system is located at a distance of 43.6 light-years from the Sun based on parallax measurements, but is drawing closer with a radial velocity of −65.6 km/s.[4] It is predicted to come as close as 15.70 light-years from the Sun in 176,900 years.[8] This star is too faint to be visible to the naked eye, having an apparent visual magnitude of +10.26[2] and an absolute magnitude of 10.24.[4]

The primary is an M-type main-sequence star with a stellar classification of M1V.[3] It is only about half the size and mass of the Sun. The star is rotating slowly with a projected rotational velocity of 0.85 km/s[4] and a rotation period of roughly 49.5 days.[6] The star has a lower metal-content compared to the Sun. It is radiating just 3%[5] of the luminosity of the Sun from its photosphere at an effective temperature of 3,493 K.[4]

A faint stellar companion was announced by E. Jódar and associates in 2013. The companion has an angular separation of 521 mas along a position angle of 352.1°±1.4° from the primary. This is equivalent to a projected separation of 7.24±0.14 AU.[9]

A planetary companion?

According to Marcy & Benitz (1989)[10] detected a possible periodicity of 510 days, inferring possible presence of a massive planetary object with minimum mass of 12 times that of Jupiter in highly eccentric orbit (e=0.6). So far the planet has not been confirmed. A radial velocity study of the star during the period 2013–2017 initially found a promising signal, but this disappeared when additional data was collected and was instead attributed to magnetic activity.[11]

The Gliese 521 planetary system[10]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b (unconfirmed) ≥12 MJ 1.038 510 0.6 — —

See also

References

  1. ^ a b c d 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.
  2. ^ a b c d e f g Jenkins, J. S.; et al. (2009). "Rotational Velocities for M Dwarfs". The Astrophysical Journal. 704 (2): 975. arXiv:0908.4092. Bibcode:2009ApJ...704..975J. doi:10.1088/0004-637X/704/2/975. S2CID 119203469.
  3. ^ a b Alonso-Floriano, F. J.; et al. (May 2015). "CARMENES input catalogue of M dwarfs. I. Low-resolution spectroscopy with CAFOS". Astronomy & Astrophysics. 577: 19. arXiv:1502.07580. Bibcode:2015A&A...577A.128A. doi:10.1051/0004-6361/201525803. A128.
  4. ^ a b c d e f g h i Houdebine, E. R. (September 2010). "Observation and modelling of main-sequence star chromospheres - XIV. Rotation of dM1 stars". Monthly Notices of the Royal Astronomical Society. 407 (3): 1657–1673. Bibcode:2010MNRAS.407.1657H. doi:10.1111/j.1365-2966.2010.16827.x.
  5. ^ a b c d e f Maldonado, J.; et al. (February 2017). "HADES RV Programme with HARPS-N at TNG . III. Flux-flux and activity-rotation relationships of early-M dwarfs". Astronomy & Astrophysics. 598: 19. arXiv:1610.05906. Bibcode:2017A&A...598A..27M. doi:10.1051/0004-6361/201629223. A27.
  6. ^ a b Suárez Mascareño, A.; et al. (April 2018). "HADES RV programme with HARPS-N at TNG. VII. Rotation and activity of M-dwarfs from time-series high-resolution spectroscopy of chromospheric indicators". Astronomy & Astrophysics. 612: 17. arXiv:1712.07375. Bibcode:2018A&A...612A..89S. doi:10.1051/0004-6361/201732143. A89.
  7. ^ "BD+46 1889". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-11-21.
  8. ^ Bailer-Jones, C. A. L. (January 2018). "The completeness-corrected rate of stellar encounters with the Sun from the first Gaia data release". Astronomy & Astrophysics. 609: 16. arXiv:1708.08595. Bibcode:2018A&A...609A...8B. doi:10.1051/0004-6361/201731453. S2CID 119462489. A8.
  9. ^ Jódar, Esther; et al. (February 2013). "New companions to nearby low-mass stars". Monthly Notices of the Royal Astronomical Society. 429 (1): 859–867. Bibcode:2013MNRAS.429..859J. doi:10.1093/mnras/sts382.
  10. ^ a b Marcy, Geoffrey W.; Benitz, Karsten J. (September 1989). "A search for substellar companions to low-mass stars". Astrophysical Journal, Part 1. 344 (1): 441–453. Bibcode:1989ApJ...344..441M. doi:10.1086/167812.
  11. ^ Gonzalez Alvarez, Ester (2018). Planets around low-mass stars and stellar activity effects. Università degli Studi di Palermo. Retrieved 2021-11-21. {{cite book}}: |work= ignored (help)
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