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{{Short description|Extrasolar planet in the Andromeda constellation}}
{{Short description|Extrasolar planet in the Andromeda constellation}}
{{Infobox planet
{{Infobox planet
| name = Upsilon Andromedae b
| name = Upsilon Andromedae b (Saffar)
| image = Size comparison - Jupiter and Upsilon Andromedae b.png
| image = Size comparison - Jupiter and Upsilon Andromedae b.png
| caption = Size comparison of Jupiter with Upsilon Andromedae b
| caption = Size comparison of Jupiter with Upsilon Andromedae b
<!-- DISCOVERY -->
<!-- DISCOVERY -->| discoverer = [[Geoffrey Marcy|Marcy]] ''et al.''
⚫
| discovery_site = [[California and Carnegie Planet Search|California and Carnegie<br/> Planet Search]]<br/>{{flag|United States}}
| discoverer = [[Geoffrey Marcy|Marcy]] ''et al.''
⚫
| discovered = June 23, 1996
⚫
| discovery_site = [[California and Carnegie Planet Search|California and Carnegie<br/> Planet Search]]<br/>{{flag|United States}}
⚫
| discovery_method = [[Radial velocity]]
⚫
| discovered = June 23, 1996
⚫
| discovery_method = [[Radial velocity]]
<!-- DESIGNATIONS -->
<!-- DESIGNATIONS -->
<!-- ORBITAL -->
<!-- ORBITAL -->| apsis = astron
| aphelion = {{val|0.0601|ul=AU}}
| apsis = astron
| aphelion = {{val|0.0601|ul=AU}}
| perihelion = {{val|0.0587|ul=AU}}
| perihelion = {{val|0.0587|ul=AU}}
| semimajor = {{val|0.0594|0.0003|ul=AU}}<ref name=Pizkorz2017/>
| semimajor = {{val|0.0594|0.0003|ul=AU}}<ref name=Pizkorz2017/>
| eccentricity = {{val|0.012|0.005}}<ref name=Pizkorz2017/>
| eccentricity = {{val|0.012|0.005}}<ref name=Pizkorz2017/>
| period = {{val|4.617111|0.000014|fmt=none|ul=d}}<ref name=Pizkorz2017/><br/>({{convert|4.617111|d|year h|disp=out|lk=on}})
| period = {{val|4.617111|0.000014|fmt=none|ul=d}}<ref name=Pizkorz2017/><br/>({{convert|4.617111|d|year h|disp=out|lk=on}})
| inclination = {{val|24|4}}<ref name=Pizkorz2017/>
| inclination = {{val|24|4}}<ref name=Pizkorz2017/>
| time_periastron = {{val|2450034.05|0.33|fmt=commas}}<ref name=Pizkorz2017/>
| time_periastron = {{val|2450034.05|0.33|fmt=commas}}<ref name=Pizkorz2017/>
| arg_peri = {{val|44.11|25.56}}<ref name=Pizkorz2017/>
| arg_peri = {{val|44.11|25.56}}<ref name=Pizkorz2017/>
| semi-amplitude = {{val|70.51|0.37}}<ref name=Pizkorz2017/>
⚫
| star = [[Upsilon Andromedae]] A
| semi-amplitude = {{val|70.51|0.37}}<ref name=Pizkorz2017/>
<!-- PHYS CHARS -->| mass = {{val|1.70|0.33|0.24}}<ref name=Pizkorz2017/> {{Jupiter mass|link=y}}
⚫
| star = [[Upsilon Andromedae]] A
⚫
| mean_radius = ~1.8<ref name=Deitrick2014/>{{Jupiter radius|link=y}}
<!-- PHYS CHARS -->
| mass = {{val|1.70|0.33|0.24}}<ref name=Pizkorz2017/> {{Jupiter mass|link=y}}
⚫
| mean_radius = ~1.8<ref name=Deitrick2014/>{{Jupiter radius|link=y}}
<!-- ATMOSPHERE -->
<!-- ATMOSPHERE -->
<!-- NOTES -->
<!-- NOTES -->}}
}}


'''Upsilon Andromedae b''' ('''υ Andromedae b''', abbreviated '''Upsilon And b''', '''υ And b'''), formally named '''Saffar''' {{IPAc-en|'|s|æ|f|ɑr}}, is an [[extrasolar planet]] approximately 44 [[light-year]]s away from the [[Sun]] in the [[constellation]] of [[Andromeda (constellation)|Andromeda]]. The planet orbits the [[solar analog]] star, [[Upsilon Andromedae]] A, approximately every five days. Discovered in June 1996 by [[Geoffrey Marcy]] and [[R. Paul Butler]], it was one of the first [[hot Jupiter]]s to be discovered. It is also one of the first non-resolved planets to be detected directly. Upsilon Andromedae b is the innermost-known planet in its [[planetary system]].
'''Upsilon Andromedae b''' ('''υ Andromedae b''', abbreviated '''Upsilon And b''', '''υ And b'''), formally named '''Saffar''' {{IPAc-en|'|s|æ|f|ɑr}}, is an [[extrasolar planet]] approximately 44 [[light-year]]s away from the [[Sun]] in the [[constellation]] of [[Andromeda (constellation)|Andromeda]]. The planet orbits the [[solar analog]] star, [[Upsilon Andromedae]] A, approximately every five days. Discovered in June 1996 by [[Geoffrey Marcy]] and [[R. Paul Butler]], it was one of the first [[hot Jupiter]]s to be discovered. It is also one of the first non-resolved planets to be detected directly. Saffar is the innermost-known planet in its [[planetary system]].


In July 2014 the [[International Astronomical Union]] launched [[NameExoWorlds]], a process for giving proper names to certain exoplanets and their host stars.<ref>[http://www.iau.org/news/pressreleases/detail/iau1404/ NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars]. IAU.org. 9 July 2014</ref> The process involved public nomination and voting for the new names.<ref>{{Cite web |url=http://nameexoworlds.iau.org/process |title=NameExoWorlds The Process |access-date=2015-09-05 |archive-date=2015-08-15 |archive-url=https://web.archive.org/web/20150815025117/http://nameexoworlds.iau.org/process |url-status=dead }}</ref> In December 2015, the IAU announced the winning name was Saffar for this planet.<ref>[http://www.iau.org/news/pressreleases/detail/iau1514/ Final Results of NameExoWorlds Public Vote Released], International Astronomical Union, 15 December 2015.</ref> The winning name was submitted by the Vega Astronomy Club of [[Morocco]] and honours the 11th-century astronomer [[Ibn al-Saffar]] of [[Muslim Spain]].<ref>{{Cite web |url=http://nameexoworlds.iau.org/names |title=NameExoWorlds The Approved Names |access-date=2016-01-17 |archive-date=2018-02-01 |archive-url=https://web.archive.org/web/20180201043609/http://nameexoworlds.iau.org/names |url-status=dead }}</ref>
In July 2014 the [[International Astronomical Union]] launched [[NameExoWorlds]], a process for giving proper names to certain exoplanets and their host stars.<ref>[http://www.iau.org/news/pressreleases/detail/iau1404/ NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars]. IAU.org. 9 July 2014</ref> The process involved public nomination and voting for the new names.<ref>{{Cite web |url=http://nameexoworlds.iau.org/process |title=NameExoWorlds The Process |access-date=2015-09-05 |archive-date=2015-08-15 |archive-url=https://web.archive.org/web/20150815025117/http://nameexoworlds.iau.org/process |url-status=dead }}</ref> In December 2015, the IAU announced the winning name was Saffar for this planet.<ref>[http://www.iau.org/news/pressreleases/detail/iau1514/ Final Results of NameExoWorlds Public Vote Released], International Astronomical Union, 15 December 2015.</ref> The winning name was submitted by the Vega Astronomy Club of [[Morocco]] and honours the 11th-century astronomer [[Ibn al-Saffar]] of [[Muslim Spain]].<ref>{{Cite web |url=http://nameexoworlds.iau.org/names |title=NameExoWorlds The Approved Names |access-date=2016-01-17 |archive-date=2018-02-01 |archive-url=https://web.archive.org/web/20180201043609/http://nameexoworlds.iau.org/names |url-status=dead }}</ref>


== Discovery ==
== Discovery ==
Upsilon Andromedae b was detected by the variations in its star's [[radial velocity]] caused by the planet's [[gravity]]. The variations were detected by making sensitive measurements of the [[Doppler shift]] of Upsilon Andromedae's [[spectrum]]. The planet's existence was announced in January 1997, together with [[55 Cancri b]] and the planet orbiting [[Tau Boötis]].<ref>{{cite journal | display-authors=1 | last1=Butler | first1=R. Paul | last2=Marcy | first2=Geoffrey W. | last3=Williams | first3=Eric | last4=Hauser | first4=Heather | last5=Shirts | first5=Phil | title=Three New 51 Pegasi-Type Planets | journal=[[The Astrophysical Journal]] | volume=474 | issue=2 | date=1997 | pages=L115–L118 | doi=10.1086/310444 | bibcode=1997ApJ...474L.115B | doi-access=free }}</ref>
Saffar was detected by the variations in its star's [[radial velocity]] caused by the planet's [[gravity]]. The variations were detected by making sensitive measurements of the [[Doppler shift]] of Upsilon Andromedae's [[spectrum]]. The planet's existence was announced in January 1997, together with [[55 Cancri b]] and the planet orbiting [[Tau Boötis]].<ref>{{cite journal | display-authors=1 | last1=Butler | first1=R. Paul | last2=Marcy | first2=Geoffrey W. | last3=Williams | first3=Eric | last4=Hauser | first4=Heather | last5=Shirts | first5=Phil | title=Three New 51 Pegasi-Type Planets | journal=[[The Astrophysical Journal]] | volume=474 | issue=2 | date=1997 | pages=L115–L118 | doi=10.1086/310444 | bibcode=1997ApJ...474L.115B | doi-access=free }}</ref>


Like [[51 Pegasi b]], the first extrasolar planet discovered around a normal star, Upsilon Andromedae b orbits very close to its star, closer than [[Mercury (planet)|Mercury]] does to the Sun. The planet takes 4.617 [[day]]s to complete an orbit, with a [[semimajor axis]] of 0.0595 [[Astronomical unit|AU]].<ref>{{cite journal | display-authors=1 |last1=Butler |first1=R. P. |last2=Wright |first2=J. T. |last3=Marcy |first3=G. W. |last4=Fischer |first4=D. A. |last5=Vogt |first5=S. S. |last6=Tinney |first6=C. G. |last7=Jones |first7=H. R. A. |last8=Carter |first8=B. D. |last9=Johnson |first9=J. A. |last10=McCarthy |first10=C. |last11=Penny |first11=A. J. | doi=10.1086/504701 | title=Catalog of Nearby Exoplanets | journal=[[The Astrophysical Journal]] | volume=646 | issue=1 | pages=505–522 | date=2006 | bibcode=2006ApJ...646..505B|arxiv = astro-ph/0607493 |s2cid=119067572 }} ([http://exoplanets.org/planets.shtml web version])</ref>
Like [[51 Pegasi b]], the first extrasolar planet discovered around a normal star, Saffar orbits very close to its star, closer than [[Mercury (planet)|Mercury]] does to the Sun. The planet takes 4.617 [[day]]s to complete an orbit, with a [[semimajor axis]] of 0.0595 [[Astronomical unit|AU]].<ref>{{cite journal | display-authors=1 |last1=Butler |first1=R. P. |last2=Wright |first2=J. T. |last3=Marcy |first3=G. W. |last4=Fischer |first4=D. A. |last5=Vogt |first5=S. S. |last6=Tinney |first6=C. G. |last7=Jones |first7=H. R. A. |last8=Carter |first8=B. D. |last9=Johnson |first9=J. A. |last10=McCarthy |first10=C. |last11=Penny |first11=A. J. | doi=10.1086/504701 | title=Catalog of Nearby Exoplanets | journal=[[The Astrophysical Journal]] | volume=646 | issue=1 | pages=505–522 | date=2006 | bibcode=2006ApJ...646..505B|arxiv = astro-ph/0607493 |s2cid=119067572 }} ([http://exoplanets.org/planets.shtml web version])</ref>


A limitation of the radial velocity method used to detect Upsilon Andromedae b is that only a lower limit on the [[mass]] can be found. The [[true mass]] may be much greater depending on the [[inclination]] of the orbit. A mass of {{Jupiter mass|link=y|1.70}} and an inclination of 24° were later found using high-resolution [[astronomical spectroscopy|spectroscopy]].<ref name=Pizkorz2017/>
A limitation of the radial velocity method used to detect Saffar is that only a lower limit on the [[mass]] can be found. The [[true mass]] may be much greater depending on the [[inclination]] of the orbit. A mass of {{Jupiter mass|link=y|1.70}} and an inclination of 24° were later found using high-resolution [[astronomical spectroscopy|spectroscopy]].<ref name=Pizkorz2017/>


== Physical characteristics ==
== Physical characteristics ==
[[File:Saffar_(Upsilon_Andromedae_b).jpg|thumb|200px|An artist's impression of Upsilon Andromedae b and its parent star]]
[[File:Saffar_(Upsilon_Andromedae_b).jpg|thumb|200px|An artist's impression of Upsilon Andromedae b and its parent star]]
Given the planet's high mass, it is likely that Upsilon Andromedae b is a [[gas giant]] with no [[solid]] surface.
Given the planet's high mass, it is likely that Saffar is a [[gas giant]] with no [[solid]] surface.


The [[Spitzer Space Telescope]] measured the planet [[temperature]], and found that the difference between the two sides of Upsilon Andromedae b of about 1,400 degrees Celsius, ranging from minus 20 to 230 degrees to about 1,400 to 1,650 °C.<ref>{{cite journal | first = J | last = Harrington |author2=Hansen BM |author3=Luszcz SH |author4=Seager S |author5=Deming D |author6=Menou K |author7=Cho JY |author8=Richardson LJ | date = October 27, 2006 | title = The phase-dependent infrared brightness of the extrasolar planet upsilon Andromedae b | journal = Science | volume = 314 | issue = 5799 | pages = 623–6 | pmid = 17038587 | doi = 10.1126/science.1133904|arxiv = astro-ph/0610491 |bibcode = 2006Sci...314..623H | s2cid = 20549014 }}</ref> The temperature difference has led to speculation that Upsilon Andromedae b is [[tidal locked]] with the same side always facing Upsilon Andromedae A.
The [[Spitzer Space Telescope]] measured the planet [[temperature]], and found that the difference between the two sides of Saffar of about 1,400 degrees Celsius, ranging from minus 20 to 230 degrees to about 1,400 to 1,650 °C.<ref>{{cite journal | first = J | last = Harrington |author2=Hansen BM |author3=Luszcz SH |author4=Seager S |author5=Deming D |author6=Menou K |author7=Cho JY |author8=Richardson LJ | date = October 27, 2006 | title = The phase-dependent infrared brightness of the extrasolar planet upsilon Andromedae b | journal = Science | volume = 314 | issue = 5799 | pages = 623–6 | pmid = 17038587 | doi = 10.1126/science.1133904|arxiv = astro-ph/0610491 |bibcode = 2006Sci...314..623H | s2cid = 20549014 }}</ref> The temperature difference has led to speculation that Saffar is [[tidal locked]] with the same side always facing Upsilon Andromedae A.


Sudarsky had, on the assumption that the planet is similar to Jupiter in composition and that its environment is close to [[chemical equilibrium]], predicted Upsilon Andromedae b to have reflective [[cloud]]s of [[silicate minerals|silicates]] and [[iron]] in its upper [[atmosphere]].<ref>{{cite journal | display-authors=1 | last1=Sudarsky | first1=David | last2=Burrows | first2=Adam | last3=Hubeny | first3=Ivan | bibcode=2003ApJ...588.1121S | title=Theoretical Spectra and Atmospheres of Extrasolar Giant Planets | journal=[[The Astrophysical Journal]] | volume=588 | issue=2 | pages=1121–1148 | date=2003 | doi=10.1086/374331 | arxiv=astro-ph/0210216 | s2cid=16004653 }}</ref> The cloud deck instead absorbs the sun's radiation; between that and the hot, high-pressure gas surrounding the mantle, exists a [[stratosphere]] of cooler gas.<ref>{{cite journal |title=Spectrum and atmosphere models of irradiated transiting extrasolar giant planets|date=2008 |author1=Ivan Hubeny |author2=Adam Burrows |doi=10.1017/S1743921308026458 |journal=Proceedings of the International Astronomical Union |volume=4 |pages=239 |arxiv=0807.3588|bibcode=2009IAUS..253..239H |s2cid=13978248 }}</ref> The outer shell of dark, opaque, hot cloud is assumed to consist of [[vanadium oxide|vanadium]] and [[titanium oxide]]s, but other compounds like [[tholin]]s cannot be ruled out yet.
Sudarsky had, on the assumption that the planet is similar to Jupiter in composition and that its environment is close to [[chemical equilibrium]], predicted Saffar to have reflective [[cloud]]s of [[silicate minerals|silicates]] and [[iron]] in its upper [[atmosphere]].<ref>{{cite journal | display-authors=1 | last1=Sudarsky | first1=David | last2=Burrows | first2=Adam | last3=Hubeny | first3=Ivan | bibcode=2003ApJ...588.1121S | title=Theoretical Spectra and Atmospheres of Extrasolar Giant Planets | journal=[[The Astrophysical Journal]] | volume=588 | issue=2 | pages=1121–1148 | date=2003 | doi=10.1086/374331 | arxiv=astro-ph/0210216 | s2cid=16004653 }}</ref> The cloud deck instead absorbs the sun's radiation; between that and the hot, high-pressure gas surrounding the mantle, exists a [[stratosphere]] of cooler gas.<ref>{{cite journal |title=Spectrum and atmosphere models of irradiated transiting extrasolar giant planets|date=2008 |author1=Ivan Hubeny |author2=Adam Burrows |doi=10.1017/S1743921308026458 |journal=Proceedings of the International Astronomical Union |volume=4 |pages=239 |arxiv=0807.3588|bibcode=2009IAUS..253..239H |s2cid=13978248 }}</ref> The outer shell of dark, opaque, hot cloud is assumed to consist of [[vanadium oxide|vanadium]] and [[titanium oxide]]s, but other compounds like [[tholin]]s cannot be ruled out yet.


The chemical elements in the atmosphere can be studied by finding their absorption lines in the thermal spectrum of the planet; given typical planet temperatures, the spectrum has its peak at infrared wavelengths. So far, only [[water vapor]] has been detected in this planet, while [[carbon monoxide]] and [[methane]] are still under the detection limit.<ref name=Pizkorz2017/>
The chemical elements in the atmosphere can be studied by finding their absorption lines in the thermal spectrum of the planet; given typical planet temperatures, the spectrum has its peak at infrared wavelengths. So far, only [[water vapor]] has been detected in this planet, while [[carbon monoxide]] and [[methane]] are still under the detection limit.<ref name=Pizkorz2017/>
Line 56: Line 52:
== Effect on the parent star ==
== Effect on the parent star ==
[[File:UAndAb full.jpg|thumb|200px|left|Artist's impression of the hot spot, shown in orange hues]]
[[File:UAndAb full.jpg|thumb|200px|left|Artist's impression of the hot spot, shown in orange hues]]
Upsilon Andromedae b appears to be responsible for increased [[chromospheric activity]] on its parent star. Observations suggest that there is a "hot spot" on the star around 169° away from the sub-planetary point. This may be the result of interactions between the [[magnetic field]]s of the planet and the star. The mechanism may be similar to that responsible for the activity of [[RS Canum Venaticorum variable]] stars, or the interaction between Jupiter and its moon [[Io (moon)|Io]].<ref>{{cite journal | url=http://www.iop.org/EJ/article/0004-637X/622/2/1075/61179.html | title=Hot Jupiters and Hot Spots: The Short- and Long-term Chromospheric Activity on Stars with Giant Planets | display-authors=1 | last1=Shkolnik | first1=E. | last2=Walker | first2=G. A. H. | last3=Bohlender | first3=D. A. | last4=Gu | first4=P.-G. | last5=Kürster | first5=M. | journal=The Astrophysical Journal | volume=622 | issue=2 | date=2005 | pages=1075–1090 | doi=10.1086/428037 | bibcode=2005ApJ...622.1075S|arxiv = astro-ph/0411655 | s2cid=3043910 }}</ref>
Saffar appears to be responsible for increased [[chromospheric activity]] on its parent star. Observations suggest that there is a "hot spot" on the star around 169° away from the sub-planetary point. This may be the result of interactions between the [[magnetic field]]s of the planet and the star. The mechanism may be similar to that responsible for the activity of [[RS Canum Venaticorum variable]] stars, or the interaction between Jupiter and its moon [[Io (moon)|Io]].<ref>{{cite journal | url=http://www.iop.org/EJ/article/0004-637X/622/2/1075/61179.html | title=Hot Jupiters and Hot Spots: The Short- and Long-term Chromospheric Activity on Stars with Giant Planets | display-authors=1 | last1=Shkolnik | first1=E. | last2=Walker | first2=G. A. H. | last3=Bohlender | first3=D. A. | last4=Gu | first4=P.-G. | last5=Kürster | first5=M. | journal=The Astrophysical Journal | volume=622 | issue=2 | date=2005 | pages=1075–1090 | doi=10.1086/428037 | bibcode=2005ApJ...622.1075S|arxiv = astro-ph/0411655 | s2cid=3043910 }}</ref>


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Revision as of 13:53, 3 July 2023

Upsilon Andromedae b (Saffar)
Size comparison of Jupiter with Upsilon Andromedae b
Discovery
Discovered byMarcy et al.
Discovery siteCalifornia and Carnegie
Planet Search
 United States
Discovery dateJune 23, 1996
Radial velocity
Orbital characteristics
Apastron0.0601 AU
Periastron0.0587 AU
0.0594±0.0003 AU[1]
Eccentricity0.012±0.005[1]
4.617111±0.000014 d[1]
(0.01264096 a; 110.8107 h)
Inclination24±4[1]
2,450,034.05±0.33[1]
44.11±25.56[1]
Semi-amplitude70.51±0.37[1]
StarUpsilon Andromedae A
Physical characteristics
~1.8[2]RJ
Mass1.70+0.33
−0.24[1] MJ

Upsilon Andromedae b (υ Andromedae b, abbreviated Upsilon And b, υ And b), formally named Saffar /ˈsæfɑːr/, is an extrasolar planet approximately 44 light-years away from the Sun in the constellation of Andromeda. The planet orbits the solar analog star, Upsilon Andromedae A, approximately every five days. Discovered in June 1996 by Geoffrey Marcy and R. Paul Butler, it was one of the first hot Jupiters to be discovered. It is also one of the first non-resolved planets to be detected directly. Saffar is the innermost-known planet in its planetary system.

In July 2014 the International Astronomical Union launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars.[3] The process involved public nomination and voting for the new names.[4] In December 2015, the IAU announced the winning name was Saffar for this planet.[5] The winning name was submitted by the Vega Astronomy Club of Morocco and honours the 11th-century astronomer Ibn al-Saffar of Muslim Spain.[6]

Discovery

Saffar was detected by the variations in its star's radial velocity caused by the planet's gravity. The variations were detected by making sensitive measurements of the Doppler shift of Upsilon Andromedae's spectrum. The planet's existence was announced in January 1997, together with 55 Cancri b and the planet orbiting Tau Boötis.[7]

Like 51 Pegasi b, the first extrasolar planet discovered around a normal star, Saffar orbits very close to its star, closer than Mercury does to the Sun. The planet takes 4.617 days to complete an orbit, with a semimajor axis of 0.0595 AU.[8]

A limitation of the radial velocity method used to detect Saffar is that only a lower limit on the mass can be found. The true mass may be much greater depending on the inclination of the orbit. A mass of 1.70 MJ and an inclination of 24° were later found using high-resolution spectroscopy.[1]

Physical characteristics

An artist's impression of Upsilon Andromedae b and its parent star

Given the planet's high mass, it is likely that Saffar is a gas giant with no solid surface.

The Spitzer Space Telescope measured the planet temperature, and found that the difference between the two sides of Saffar of about 1,400 degrees Celsius, ranging from minus 20 to 230 degrees to about 1,400 to 1,650 °C.[9] The temperature difference has led to speculation that Saffar is tidal locked with the same side always facing Upsilon Andromedae A.

Sudarsky had, on the assumption that the planet is similar to Jupiter in composition and that its environment is close to chemical equilibrium, predicted Saffar to have reflective clouds of silicates and iron in its upper atmosphere.[10] The cloud deck instead absorbs the sun's radiation; between that and the hot, high-pressure gas surrounding the mantle, exists a stratosphere of cooler gas.[11] The outer shell of dark, opaque, hot cloud is assumed to consist of vanadium and titanium oxides, but other compounds like tholins cannot be ruled out yet.

The chemical elements in the atmosphere can be studied by finding their absorption lines in the thermal spectrum of the planet; given typical planet temperatures, the spectrum has its peak at infrared wavelengths. So far, only water vapor has been detected in this planet, while carbon monoxide and methane are still under the detection limit.[1]

The planet is unlikely to have large moons, since tidal forces would either eject them from orbit or destroy them on short timescales compared to the age of the system.[12]

The planet (with 51 Pegasi b) was deemed a candidate for direct imaging by Planetpol.[13] Preliminary results from polarimetric studies indicate that the planet has predominately blue color, is 1.36 times as large and 0.74 times as massive as Jupiter, meaning that the mean density is 0.36g/cm3. It has a geometric albedo of 0.35 in visible light.[14] In 2016–2017 the direct detection of the planetary thermal emission was claimed, but the detection was questioned in 2021.[15] Tidal heating models predict a similar mass for the planet.[2]

Effect on the parent star

Artist's impression of the hot spot, shown in orange hues

Saffar appears to be responsible for increased chromospheric activity on its parent star. Observations suggest that there is a "hot spot" on the star around 169° away from the sub-planetary point. This may be the result of interactions between the magnetic fields of the planet and the star. The mechanism may be similar to that responsible for the activity of RS Canum Venaticorum variable stars, or the interaction between Jupiter and its moon Io.[16]

See also

References

  1. ^ a b c d e f g h i j Pizkorz, D.; et al. (August 2017). "Detection of Water Vapor in the Thermal Spectrum of the Non-transiting Hot Jupiter Upsilon Andromedae b". The Astronomical Journal. 154 (2): 78. arXiv:1707.01534. Bibcode:2017AJ....154...78P. doi:10.3847/1538-3881/aa7dd8. S2CID 19960378.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  2. ^ a b Deitrick, R.; et al. (January 2015). "The Three-dimensional Architecture of the υ Andromedae Planetary System". The Astrophysical Journal. 798 (1): 46. arXiv:1411.1059. Bibcode:2015ApJ...798...46D. doi:10.1088/0004-637X/798/1/46. S2CID 118409453.
  3. ^ NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars. IAU.org. 9 July 2014
  4. ^ "NameExoWorlds The Process". Archived from the original on 2015-08-15. Retrieved 2015-09-05.
  5. ^ Final Results of NameExoWorlds Public Vote Released, International Astronomical Union, 15 December 2015.
  6. ^ "NameExoWorlds The Approved Names". Archived from the original on 2018-02-01. Retrieved 2016-01-17.
  7. ^ Butler, R. Paul; et al. (1997). "Three New 51 Pegasi-Type Planets". The Astrophysical Journal. 474 (2): L115–L118. Bibcode:1997ApJ...474L.115B. doi:10.1086/310444.
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