Gliese 49: Difference between revisions

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'''Gliese 49''' ([[Gliese Catalog|GJ]] 49 / [[Hipparcos Catalog|HIP]] 4872)<ref name="SIMBAD">[http://simbad.u-strasbg.fr/simbad/sim-id?protocol=html&Ident=Gliese+49&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id LHS 1179 -- High proper-motion Star] ([[SIMBAD]])</ref> is a [[star]] in the [[constellation]] of [[Cassiopeia (constellation)|Cassiopeia]]. Visually, it is located 106 arc minutes north of the bright star [[Gamma Cassiopeiae|γ Cassiopeiae]]. With an [[apparent magnitude]] of 9.56,<ref name="SIMBAD" /> is not observable with the naked eye. It is located, based on the reduction of [[parallax]] data of [[Hipparcos]] (100.40 ± 1.52 [[Minute and second of arc|Millisecond of arc]]), 32.5 [[light-year]]s away from the [[Solar System]].
'''Gliese 49''' ([[Gliese Catalog|GJ]] 49 / [[Hipparcos Catalog|HIP]] 4872)<ref name="SIMBAD">[http://simbad.u-strasbg.fr/simbad/sim-id?protocol=html&Ident=Gliese+49&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id LHS 1179 -- High proper-motion Star] ([[SIMBAD]])</ref> is a [[star]] in the [[constellation]] of [[Cassiopeia (constellation)|Cassiopeia]]. Visually, it is located 106 arc minutes north of the bright star [[Gamma Cassiopeiae|γ Cassiopeiae]]. With an [[apparent magnitude]] of 9.56,<ref name="SIMBAD" /> is not observable with the naked eye. It is located, based on the reduction of [[parallax]] data of [[Hipparcos]] (100.40 ± 1.52 [[Minute and second of arc|Millisecond of arc]]), 32.5 [[light-year]]s away from the [[Solar System]].


Gliese 49 is a [[red dwarf]] of [[spectral type]] M1.5V. Much dimmer than [[Sun]], it has a total [[luminosity]] that is 5.0% that of the [[solar luminosity|Sun]];<ref>{{cita publicación|autor=Morales, J. C.; Ribas, I.; Jordi, C.|título=The effect of activity on stellar temperatures and radii|año=2008|publicación=[[Astronomy and Astrophysics]]|volumen=478|número=2|id=pp. 507-512|url=http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2008A%26A...478..507M&db_key=AST&nosetcookie=1}}</ref> it is, however, much brighter than other nearby red dwarfs such as [[Proxima Centauri]] or [[Wolf 359]]. It has an [[effective temperature]] of 3454 ± 50 [[Kelvin|K]]. Its mass is 57% that of the Sun and its radius is 2/3 that of the Sun.
Gliese 49 is a [[red dwarf]] of [[spectral type]] M1.5V. Much dimmer than [[Sun]], it has a total [[luminosity]] that is 5.0% that of the [[solar luminosity|Sun]];<ref>{{cita publicación|autor=Morales, J. C.; Ribas, I.; Jordi, C.|título=The effect of activity on stellar temperatures and radii|año=2008|publicación=[[Astronomy and Astrophysics]] | volumen=478|número=2|id=pp. 507-512|url=http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2008A%26A...478..507M&db_key=AST&nosetcookie=1}}</ref> it is, however, much brighter than other nearby red dwarfs such as [[Proxima Centauri]] or [[Wolf 359]]. It has an [[effective temperature]] of 3454 ± 50 [[Kelvin|K]]. Its mass is 57% that of the Sun and its radius is 2/3 that of the Sun.


It rotates on its axis with a projected rotation speed of 2.5&nbsp;km/s, which means that its [[rotation period]] does not exceed 13.4 days. It has a metallic content similar to that of the Sun, with its index of [[metallicity]] [M / H] = +0.03.<ref name="Houdebine">{{cita publicación|autor=Houdebine, E. R.|título=Observation and modelling of main-sequence star chromospheres - XIV. Rotation of dM1 stars|año=2010|publicación=[[Monthly Notices of the Royal Astronomical Society]]|volumen=407|número=3|id=pp. 1657-1673|url=http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2010MNRAS.407.1657H&db_key=AST&nosetcookie=1}}</ref> Although its age is not known exactly, it is less than 250 million years.
It rotates on its axis with a projected rotation speed of 2.5&nbsp;km/s, which means that its [[rotation period]] does not exceed 13.4 days. It has a metallic content similar to that of the Sun, with its index of [[metallicity]] [M / H] = +0.03.<ref name="Houdebine">{{cita publicación|autor=Houdebine, E. R.|título=Observation and modelling of main-sequence star chromospheres – XIV. Rotation of dM1 stars|año=2010|publicación=[[Monthly Notices of the Royal Astronomical Society]] | volumen=407|número=3|id=pp. 1657–1673|url=http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2010MNRAS.407.1657H&db_key=AST&nosetcookie=1}}</ref> Although its age is not known exactly, it is less than 250 million years.


Gliese 49 has a similar [[proper motion]] to the red dwarf [[flare star]] [[V388 Cassiopeiae]]. The visual separation between the two is 295 [[Arcsec|arcseconds]], which implies that the real distance between them is over 2900 [[Astronomical unit|AU]]. Both stars are associated with the [[Hyades (astronomy)|Hyades]], as suggested by its young age and chromospheric activity levels.<ref name="Makarov">{{cita publicación|autor=Makarov, V. V.; Zacharias, N.; Hennessy, G. S.|título=Common Proper Motion Companions to Nearby Stars: Ages and Evolution|año=2008|publicación=[[The Astrophysical Journal]]|volumen=687|número=1|id=pp. 566-578|url=http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2008ApJ...687..566M&db_key=AST&nosetcookie=1}}</ref>
Gliese 49 has a similar [[proper motion]] to the red dwarf [[flare star]] [[V388 Cassiopeiae]]. The visual separation between the two is 295 [[arcsec]]onds, which implies that the real distance between them is over 2900 [[Astronomical unit|AU]]. Both stars are associated with the [[Hyades (astronomy)|Hyades]], as suggested by its young age and chromospheric activity levels.<ref name="Makarov">{{cita publicación|autor=Makarov, V. V.; Zacharias, N.; Hennessy, G. S.|título=Common Proper Motion Companions to Nearby Stars: Ages and Evolution|año=2008|publicación=[[The Astrophysical Journal]] | volumen=687|número=1|id=pp. 566-578|url=http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2008ApJ...687..566M&db_key=AST&nosetcookie=1}}</ref>


== Planetary System ==
== Planetary system ==
One known planet is known to orbit Gliese 49. Gliese 49 b is a [[super-Earth]] planet detected by the [[radial velocity method]].<ref>{{Cite journal|last=Perger|first=M.|last2=Scandariato|first2=G.|last3=Ribas|first3=I.|last4=Morales|first4=J. C.|last5=Affer|first5=L.|last6=Azzaro|first6=M.|last7=Amado|first7=P. J.|last8=Anglada-Escudé|first8=G.|last9=Baroch|first9=D.|date=2019-03-15|title=Gliese 49: Activity evolution and detection of a super-Earth|url=http://arxiv.org/abs/1903.04808|journal=Astronomy & Astrophysics|doi=10.1051/0004-6361/201935192|issn=0004-6361}}</ref><ref>{{Cite web|url=https://arxiv.org/pdf/1903.04808.pdf|title=Gliese 49: Activity evolution and detection of a super-Earth? A HADES and CARMENES collaboration|last=|first=|date=25 March 2019|website=|archive-url=|archive-date=|dead-url=|access-date=}}</ref>
One known planet is known to orbit Gliese 49. Gliese 49 b is a [[super-Earth]] planet detected by the [[radial velocity method]].<ref>{{Cite journal |last=Perger |first=M. |last2=Scandariato |first2=G. |last3=Ribas |first3=I. |last4=Morales |first4=J. C. |last5=Affer |first5=L. |last6=Azzaro |first6=M. |last7=Amado |first7=P. J. |last8=Anglada-Escudé |first8=G. |last9=Baroch |first9=D. |date=2019-03-15 |title=Gliese 49: Activity evolution and detection of a super-Earth |url=http://arxiv.org/abs/1903.04808 |journal=Astronomy & Astrophysics |doi=10.1051/0004-6361/201935192 |issn=0004-6361}}</ref><ref>{{Cite web |url=https://arxiv.org/pdf/1903.04808.pdf |title=Gliese 49: Activity evolution and detection of a super-Earth? A HADES and CARMENES collaboration |last= |first= |date=25 March 2019 |website= |archive-url= |archive-date= |dead-url= |access-date=}}</ref>


{{OrbitboxPlanet begin}}
{{OrbitboxPlanet begin}}
{{OrbitboxPlanet|exoplanet=[[Gliese 49 b|b]]|mass_earth={{val|5.63|+0.67|−0.68}}|period={{val|13.8508|+0.0053|−0.0051}}|semimajor=0.0905 ± 0.0011|eccentricity={{val|0.363|+0.099|−0.096}}}}
{{OrbitboxPlanet|exoplanet=[[Gliese 49 b|b]] | mass_earth={{val|5.63|+0.67|−0.68}}|period={{val|13.8508|+0.0053|−0.0051}}|semimajor=0.0905 ± 0.0011|eccentricity={{val|0.363|+0.099|−0.096}}}}
{{Orbitbox end}}
{{Orbitbox end}}


Revision as of 07:29, 31 March 2019

Gliese 49 (GJ 49 / HIP 4872)[1] is a star in the constellation of Cassiopeia. Visually, it is located 106 arc minutes north of the bright star γ Cassiopeiae. With an apparent magnitude of 9.56,[1] is not observable with the naked eye. It is located, based on the reduction of parallax data of Hipparcos (100.40 ± 1.52 Millisecond of arc), 32.5 light-years away from the Solar System.

Gliese 49 is a red dwarf of spectral type M1.5V. Much dimmer than Sun, it has a total luminosity that is 5.0% that of the Sun;[2] it is, however, much brighter than other nearby red dwarfs such as Proxima Centauri or Wolf 359. It has an effective temperature of 3454 ± 50 K. Its mass is 57% that of the Sun and its radius is 2/3 that of the Sun.

It rotates on its axis with a projected rotation speed of 2.5 km/s, which means that its rotation period does not exceed 13.4 days. It has a metallic content similar to that of the Sun, with its index of metallicity [M / H] = +0.03.[3] Although its age is not known exactly, it is less than 250 million years.

Gliese 49 has a similar proper motion to the red dwarf flare star V388 Cassiopeiae. The visual separation between the two is 295 arcseconds, which implies that the real distance between them is over 2900 AU. Both stars are associated with the Hyades, as suggested by its young age and chromospheric activity levels.[4]

Planetary system

One known planet is known to orbit Gliese 49. Gliese 49 b is a super-Earth planet detected by the radial velocity method.[5][6]

The Gliese 49 planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b 5.63+0.67
−0.68 M🜨 		0.0905 ± 0.0011 13.8508+0.0053
−0.0051 		0.363+0.099
−0.096 		— —

References

  1. ^ a b LHS 1179 -- High proper-motion Star (SIMBAD)
  2. ^ Morales, J. C.; Ribas, I.; Jordi, C. (2008). "The effect of activity on stellar temperatures and radii". Astronomy and Astrophysics. 478 (2). pp. 507-512.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  3. ^ Houdebine, E. R. (2010). "Observation and modelling of main-sequence star chromospheres – XIV. Rotation of dM1 stars". Monthly Notices of the Royal Astronomical Society. 407 (3). pp. 1657–1673.
  4. ^ Makarov, V. V.; Zacharias, N.; Hennessy, G. S. (2008). "Common Proper Motion Companions to Nearby Stars: Ages and Evolution". The Astrophysical Journal. 687 (1). pp. 566-578.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  5. ^ Perger, M.; Scandariato, G.; Ribas, I.; Morales, J. C.; Affer, L.; Azzaro, M.; Amado, P. J.; Anglada-Escudé, G.; Baroch, D. (2019-03-15). "Gliese 49: Activity evolution and detection of a super-Earth". Astronomy & Astrophysics. doi:10.1051/0004-6361/201935192. ISSN 0004-6361.
  6. ^ "Gliese 49: Activity evolution and detection of a super-Earth? A HADES and CARMENES collaboration" (PDF). 25 March 2019. {{cite web}}: Cite has empty unknown parameter: |dead-url= (help)
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