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Coordinates: Sky map 08h 36m 23.0163s, −30° 02′ 15.442″
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{{Short description|Variable G-type star in the constellation Pyxis}}
{{Short description|Star in the constellation Pyxis}}
{{Distinguish|HD 73526}}
{{Starbox begin}}
{{Starbox begin}}
{{Starbox observe
{{Starbox observe
| epoch = J2000.0
| epoch = J2000.0
| constell = [[Pyxis]]
| constell = [[Pyxis]]
| ra = {{RA|08|36|23.01633}}<ref name=GaiaDR2/>
| ra = {{RA|08|36|23.01654}}<ref name=GaiaDR3/>
| dec = {{DEC|−30|02|15.4419}}<ref name=GaiaDR2/>
| dec = {{DEC|−30|02|15.4462}}<ref name=GaiaDR3/>
| appmag_v = 8.08<ref name=Anderson_Francis_2012/>
| appmag_v = 8.08<ref name=Anderson_Francis_2012/>
}}
}}
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}}
}}
{{Starbox astrometry
{{Starbox astrometry
| radial_v = {{val|+29.77|0.22}}<ref name=Anderson_Francis_2012/>
| radial_v = {{val|29.66|0.14}}<ref name=GaiaDR3/>
| prop_mo_ra = −182.015<ref name=GaiaDR2/>
| prop_mo_ra = {{val|−182.193|(17)}}
| prop_mo_dec = +67.080<ref name=GaiaDR2/>
| prop_mo_dec = {{val|67.373|(21)}}
⚫
| pm_footnote = <ref name=GaiaDR3/>
⚫
| parallax = 27.2131
| p_error = 0.0413
| parallax = 27.2441
⚫
| p_error = 0.0217
⚫
| parallax_footnote = <ref name=GaiaDR2/>
| parallax_footnote = <ref name=GaiaDR3/>
| absmag_v = 5.20<ref name=Anderson_Francis_2012/>
| absmag_v = 5.20<ref name=Anderson_Francis_2012/>
}}
}}
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}}
}}
{{Starbox catalog
{{Starbox catalog
| names = {{odlist | V=CS Pyx | BD=−29°6456 | HD=73256 | HIP=42214 | SAO=176159 }}<ref name=SIMBAD/>
| names = {{odlist | V=CS Pyx | CD=−29°6456 | HD=73256 | HIP=42214 | SAO=176159 }}<ref name=SIMBAD/>
}}
}}
{{Starbox reference
{{Starbox reference
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{{Starbox end}}
{{Starbox end}}


'''HD 73256''' is a [[variable star]] in the southern [[constellation]] of [[Pyxis]]. It has the [[variable star designation]] '''CS Pyxidis'''. With a baseline [[apparent visual magnitude]] of 8.08,<ref name=Anderson_Francis_2012/> it requires a small telescope to view. The star is located at a distance of 120&nbsp;[[light year]]s from the [[Sun]] based on [[stellar parallax|parallax]],<ref name=GaiaDR2/> and is drifting further away with a [[radial velocity]] of +30&nbsp;km/s.<ref name=Anderson_Francis_2012/>
'''HD 73256''' is a [[variable star]] in the southern [[constellation]] of [[Pyxis]]. It has the [[variable star designation]] '''CS Pyxidis'''. With a baseline [[apparent visual magnitude]] of 8.08,<ref name=Anderson_Francis_2012/> it requires [[binoculars]] or a small telescope to view. The star is located at a distance of 120&nbsp;[[light year]]s from the [[Sun]] based on [[stellar parallax|parallax]],<ref name=GaiaDR3/> and is drifting further away with a [[radial velocity]] of +30&nbsp;km/s.<ref name=Anderson_Francis_2012/>


The [[stellar classification]] of this star is G8IV-VFe+0.5, which suggests a slightly evolved [[G-type main-sequence star]] with a mild overabundance of iron in the spectrum. It is a [[BY Draconis variable]] with a period of 13.97&nbsp;days, showing a variation of 0.03 in magnitude due to [[chromospheric activity]].<ref name=Samus_et_al_2017/> The star appears overluminous for its class, which may be the result of a high [[metallicity]].<ref name="Udry2003"/> The star has roughly the same mass and a slightly smaller radius as the Sun, but is radiating 74% of the Sun's luminosity.<ref name="Bonfanti2015"/> It is around 2–3&nbsp;billion years old and is spinning with a [[projected rotational velocity]] of 3.2&nbsp;km/s.<ref name="Udry2003"/>
The [[stellar classification]] of this star is G8IV-VFe+0.5, which suggests a slightly evolved [[G-type main-sequence star]] with a mild overabundance of iron in the spectrum. It is a [[BY Draconis variable]] with a period of 13.97&nbsp;days, showing a variation of 0.03 in magnitude due to [[chromospheric activity]].<ref name=Samus_et_al_2017/> The star appears overluminous for its class, which may be the result of a high [[metallicity]].<ref name="Udry2003"/> The star has roughly the same mass and a slightly smaller radius as the Sun, but is radiating 74% of the Sun's luminosity.<ref name="Bonfanti2015"/> It is around 2–3&nbsp;billion years old and is spinning with a [[projected rotational velocity]] of 3.2&nbsp;km/s.<ref name="Udry2003"/>


==Planetary system==
⚫
In 2003, S. Udry and colleagues reported the discovery of a planet in orbit around HD 73256 using data from the [[CORALIE spectrograph]]. This object is a [[Hot Jupiter]] with at least 1.87 times the [[mass of Jupiter]] in an orbit with a period of 2.55&nbsp;days.<ref name="Udry2003"/> In 2018, K. Ment and colleagues reported an attempt to confirm the existence of this planet using Keck/HIRES data, but were unable to do so. Thus the existence of this object is disputed.<ref name=Ment_et_al_2018/>
In 2003, S. Udry and colleagues reported the discovery of a planet in orbit around HD 73256 using data from the [[CORALIE spectrograph]]. This object is a [[hot Jupiter]] with at least 1.87 times the [[mass of Jupiter]] in an orbit with a period of 2.55&nbsp;days.<ref name="Udry2003"/> Assuming the planet is perfectly grey with no greenhouse or tidal effects, and a Bond albedo of 0.1, the temperature would be about 1300 [[Kelvin|K]]. This is close to [[51 Pegasi b]]; between the predicted temperatures of [[HD 189733 b]] and [[HD 209458 b]] (1180-1392K), before they were measured. It is a candidate for "near-infrared characterisation with the VLTI Spectro-Imager".<ref>{{cite journal |doi=10.1117/12.790494 |journal=Proceedings of SPIE |date=2008 |last1=Renard |first1=Stéphanie |last2=Absil |first2=Olivier |last3=Berger |first3=Jean-Philippe |last4=Bonfils |first4=Xavier |last5=Forveille |first5=Thierry |last6=Malbet |first6=Fabien | title=Prospects for near-infrared characterisation of hot Jupiters with the VLTI Spectro-Imager (VSI) |series=Optical and Infrared Interferometry |volume=7013 |pages=70132Z–70132Z–10 |arxiv=0807.3014 |url=http://orbi.ulg.ac.be/bitstream/2268/30158/1/SPIE_poster.pdf |bibcode=2008SPIE.7013E..2ZR |s2cid=119268109 }}</ref>

⚫
In 2018, K. Ment and colleagues reported an attempt to confirm the existence of this planet using Keck/HIRES data, but were unable to do so despite a likelihood of success. Thus the existence of this object is disputed.<ref name=Ment_et_al_2018/>

In 2023, a different substellar companion on a wide orbit, likely a [[brown dwarf]], was discovered using both radial velocity and [[astrometry]]. This study did also detect HD 73256 b, but did not update its parameters or address the dispute.<ref name="Philipot2023"/>


{{OrbitboxPlanet begin
{{OrbitboxPlanet begin
| table_ref = <ref name="Udry2003"/>
| table_ref = <ref name="Udry2003"/><ref name="Philipot2023"/>
}}
}}
{{OrbitboxPlanet
{{OrbitboxPlanet hypothetical
| exoplanet = [[HD 73256 b|b]]
| exoplanet = b
| mass = >1.87 ± 0.49
| mass = >1.87 ± 0.49
| period = 2.54858 ± 0.00016
| period = 2.54858 ± 0.00016
| semimajor = 0.037
| semimajor = 0.037
| eccentricity = 0.029 ± 0.02
| eccentricity = 0.029 ± 0.02
| status = disputed
}}
{{OrbitboxPlanet
| exoplanet = c
| mass = {{val|16|1}}
| period = {{val|2690|60|102}}
| semimajor = {{val|3.8|0.1}}
| eccentricity = {{val|0.16|0.07}}
| inclination = {{val|29|5|3}} or {{val|152|8|7}}
}}
}}
{{Orbitbox end}}
{{Orbitbox end}}
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{{Reflist|refs=
{{Reflist|refs=


<ref name=GaiaDR2>{{Cite Gaia DR2|5643762781311698048}}</ref>
<ref name=GaiaDR3>{{Cite Gaia DR3|5643762781311698048}}</ref>


<ref name=SIMBAD>{{cite simbad
<ref name=SIMBAD>{{cite simbad
Line 134: Line 150:
| volume=156 | issue=5 | id=213 | pages=45 | date=November 2018
| volume=156 | issue=5 | id=213 | pages=45 | date=November 2018
| arxiv=1809.01228 | bibcode=2018AJ....156..213M
| arxiv=1809.01228 | bibcode=2018AJ....156..213M
| doi=10.3847/1538-3881/aae1f5 | s2cid=119243619 }}</ref>
| doi=10.3847/1538-3881/aae1f5 | s2cid=119243619 | doi-access=free }}</ref>

<ref name="Philipot2023">{{cite journal |last1=Philipot |first1=F. |last2=Lagrange |first2=A.-M. |display-authors=etal |date=August 2023 |title=Multi techniques approach to identify and/or constrain radial velocity sub-stellar companions |journal=[[Astronomy & Astrophysics]] |volume= |issue= |pages= |doi= 10.1051/0004-6361/202346612|arxiv=2308.05417|s2cid=260775968 }}</ref>


}}
}}
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[[Category:G-type main-sequence stars]]
[[Category:G-type main-sequence stars]]
[[Category:G-type subgiants]]
[[Category:G-type subgiants]]
[[Category:Planetary systems with one confirmed planet]]
[[Category:Hypothetical planetary systems]]
[[Category:BY Draconis variables]]
[[Category:BY Draconis variables]]
<!-- Identifiers -->
<!-- Identifiers -->
[[Category:Pyxis (constellation)]]
[[Category:Pyxis]]
[[Category:Durchmusterung objects]]
[[Category:Durchmusterung objects|CD-29 06456]]
[[Category:Henry Draper Catalogue objects|073256]]
[[Category:Henry Draper Catalogue objects|073256]]
[[Category:Hipparcos objects|042214]]
[[Category:Hipparcos objects|042214]]

Latest revision as of 00:07, 28 November 2023

Not to be confused with HD 73526.
HD 73256
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Pyxis
Right ascension 08h 36m 23.01654s[1]
Declination −30° 02′ 15.4462″[1]
Apparent magnitude (V) 8.08[2]
Characteristics
Spectral type G8 IV-V Fe+0.5[3]
B−V color index 0.782±0.002[2]
Variable type BY Dra[4]
Astrometry
Radial velocity (Rv)29.66±0.14[1] km/s
Proper motion (μ) RA: −182.193(17) mas/yr[1]
Dec.: 67.373(21) mas/yr[1]
Parallax (π)27.2441 ± 0.0217 mas[1]
Distance119.72 ± 0.10 ly
(36.71 ± 0.03 pc)
Absolute magnitude (MV)5.20[2]
Details[5]
Mass1.01±0.03 M☉
Radius0.94±0.02 R☉
Luminosity0.74±0.01 L☉
Surface gravity (log g)4.49±0.03 cgs
Temperature5,532±36 K
Metallicity [Fe/H]0.29±0.05[6] dex
Rotational velocity (v sin i)3.22±0.32[6] km/s
Age2.5±2.3 Gyr
Other designations
CS Pyx, CD−29°6456, HD 73256, HIP 42214, SAO 176159[7]
Database references
SIMBADdata

HD 73256 is a variable star in the southern constellation of Pyxis. It has the variable star designation CS Pyxidis. With a baseline apparent visual magnitude of 8.08,[2] it requires binoculars or a small telescope to view. The star is located at a distance of 120 light years from the Sun based on parallax,[1] and is drifting further away with a radial velocity of +30 km/s.[2]

The stellar classification of this star is G8IV-VFe+0.5, which suggests a slightly evolved G-type main-sequence star with a mild overabundance of iron in the spectrum. It is a BY Draconis variable with a period of 13.97 days, showing a variation of 0.03 in magnitude due to chromospheric activity.[4] The star appears overluminous for its class, which may be the result of a high metallicity.[6] The star has roughly the same mass and a slightly smaller radius as the Sun, but is radiating 74% of the Sun's luminosity.[5] It is around 2–3 billion years old and is spinning with a projected rotational velocity of 3.2 km/s.[6]

Planetary system

[edit]

In 2003, S. Udry and colleagues reported the discovery of a planet in orbit around HD 73256 using data from the CORALIE spectrograph. This object is a hot Jupiter with at least 1.87 times the mass of Jupiter in an orbit with a period of 2.55 days.[6] Assuming the planet is perfectly grey with no greenhouse or tidal effects, and a Bond albedo of 0.1, the temperature would be about 1300 K. This is close to 51 Pegasi b; between the predicted temperatures of HD 189733 b and HD 209458 b (1180-1392K), before they were measured. It is a candidate for "near-infrared characterisation with the VLTI Spectro-Imager".[8]

In 2018, K. Ment and colleagues reported an attempt to confirm the existence of this planet using Keck/HIRES data, but were unable to do so despite a likelihood of success. Thus the existence of this object is disputed.[9]

In 2023, a different substellar companion on a wide orbit, likely a brown dwarf, was discovered using both radial velocity and astrometry. This study did also detect HD 73256 b, but did not update its parameters or address the dispute.[10]

The HD 73256 planetary system[6][10]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b (disputed) >1.87 ± 0.49 MJ 0.037 2.54858 ± 0.00016 0.029 ± 0.02 — —
c 16±1 MJ 3.8±0.1 2690+60
−102 		0.16±0.07 29+5
−3 or 152+8
−7° 		—

See also

[edit]

References

[edit]
  1. ^ a b c d e f Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b c d e Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  3. ^ Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID 119476992.
  4. ^ a b Samus, N. N.; et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
  5. ^ a b Bonfanti, A.; et al. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics. 575. A18. arXiv:1411.4302. Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951. S2CID 54555839.
  6. ^ a b c d e f Udry, S.; et al. (2003). "The CORALIE survey for southern extra-solar planets X. A Hot Jupiter orbiting HD 73256". Astronomy and Astrophysics. 407 (2): 679–684. arXiv:astro-ph/0304248. Bibcode:2003A&A...407..679U. doi:10.1051/0004-6361:20030815. S2CID 118889984.
  7. ^ "HD 73256". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-11-28.
  8. ^ Renard, Stéphanie; Absil, Olivier; Berger, Jean-Philippe; Bonfils, Xavier; Forveille, Thierry; Malbet, Fabien (2008). "Prospects for near-infrared characterisation of hot Jupiters with the VLTI Spectro-Imager (VSI)" (PDF). Proceedings of SPIE. Optical and Infrared Interferometry. 7013: 70132Z–70132Z–10. arXiv:0807.3014. Bibcode:2008SPIE.7013E..2ZR. doi:10.1117/12.790494. S2CID 119268109.
  9. ^ Ment, Kristo; et al. (November 2018). "Radial Velocities from the N2K Project: Six New Cold Gas Giant Planets Orbiting HD 55696, HD 98736, HD 148164, HD 203473, and HD 211810". The Astronomical Journal. 156 (5): 45. arXiv:1809.01228. Bibcode:2018AJ....156..213M. doi:10.3847/1538-3881/aae1f5. S2CID 119243619. 213.
  10. ^ a b Philipot, F.; Lagrange, A.-M.; et al. (August 2023). "Multi techniques approach to identify and/or constrain radial velocity sub-stellar companions". Astronomy & Astrophysics. arXiv:2308.05417. doi:10.1051/0004-6361/202346612. S2CID 260775968.


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