Editing Exoplanet (section)

=== Rings ===
In 2007, the star [[V1400 Centauri]] was occulted by an object (either a planet or brown dwarf) surrounded by an extensive disc of debris. The object, designated [[J1407b]], was long believed to host a vast planetary [[ring system]] much larger than [[Saturn's rings]].<ref>{{Cite web|title=Scientists Discover a Saturn-like Ring System Eclipsing a Sun-like Star|url=https://www.spacedaily.com/reports/Scientists_Discover_a_Saturn_like_Ring_System_Eclipsing_a_Sun_like_Star_999.html|access-date=2022-01-17|website=www.spacedaily.com}}</ref><ref>{{Cite journal | doi = 10.1088/0004-6256/143/3/72| title = Planetary Construction Zones in Occultation: Discovery of an Extrasolar Ring System Transiting a Young Sun-Like Star and Future Prospects for Detecting Eclipses by Circumsecondary and Circumplanetary Disks| journal = The Astronomical Journal| volume = 143| issue = 3| page = 72| year = 2012| last1 = Mamajek | first1 = E. E. | last2 = Quillen | first2 = A. C. | last3 = Pecaut | first3 = M. J. | last4 = Moolekamp | first4 = F. | last5 = Scott | first5 = E. L. | last6 = Kenworthy | first6 = M. A. | last7 = Cameron | first7 = A. C. | last8 = Parley | first8 = N. R. | bibcode=2012AJ....143...72M|arxiv = 1108.4070 | s2cid = 55818711}}</ref> Follow-up observations found the supposed ring system could instead be a circumplanetary disk.<ref>{{cite journal |last1=Rieder |first1=Steven |last2=Kenworthy |first2=Matthew A. |date=November 2016 |title=Constraints on the size and dynamics of the J1407b ring system |journal=Astronomy & Astrophysics |volume=596 |pages=5 |arxiv=1609.08485 |bibcode=2016A&A...596A...9R |doi=10.1051/0004-6361/201629567 |s2cid=118413749 |id=A9 |doi-access=free}}</ref><ref>{{cite journal |last1=Kenworthy |first1=M. A. |last2=Klaasen |first2=P. D. |last3=Min |first3=M. |last4=van der Marel |first4=N. |last5=Bohn |first5=A. J. |last6=Kama |first6=M. |display-authors=etal |date=January 2020 |title=ALMA and NACO observations towards the young exoring transit system J1407 (V1400 Cen) |journal=Astronomy & Astrophysics |volume=633 |pages=6 |arxiv=1912.03314 |bibcode=2020A&A...633A.115K |doi=10.1051/0004-6361/201936141 |id=A115 |doi-access=free}}</ref>

There is strong evidence of a ring system around [[HIP 41378 f]], given the planet's measured radius is too large for its mass, the radius measurement might have been affected by a ring system around the planet.<ref name="Saillenfest2023">{{Cite journal |last1=Saillenfest |first1=M. |last2=Sulis |first2=S. |last3=Charpentier |first3=P. |last4=Santerne |first4=A. |year=2023 |title=Oblique rings from migrating exomoons: A possible origin for long-period exoplanets with enlarged radii |journal=Astronomy and Astrophysics |volume=675 |doi=10.1051/0004-6361/20234674 |doi-broken-date=1 November 2024}}</ref><ref>{{cite journal |last1=Alam |first1=Munazza K. |last2=Kirk |first2=James |last3=Dressing |first3=Courtney D. |last4=López-Morales |first4=Mercedes |last5=Ohno |first5=Kazumasa |last6=Gao |first6=Peter |last7=Akinsanmi |first7=Babatunde |last8=Santerne |first8=Alexandre |last9=Grouffal |first9=Salomé |last10=Adibekyan |first10=Vardan |last11=Barros |first11=Susana C. C. |last12=Buchhave |first12=Lars A. |last13=Crossfield |first13=Ian J. M. |last14=Dai |first14=Fei |last15=Deleuil |first15=Magali |year=2022 |title=The First Near-infrared Transmission Spectrum of HIP 41378 f, A Low-mass Temperate Jovian World in a Multiplanet System |journal=The Astrophysical Journal Letters |volume=927 |issue=1 |pages=L5 |arxiv=2201.02686 |bibcode=2022ApJ...927L...5A |doi=10.3847/2041-8213/ac559d |s2cid=245837282 |doi-access=free |last16=Giacalone |first16=Steven |last17=Lillo-Box |first17=Jorge |last18=Marley |first18=Mark |last19=Mayo |first19=Andrew W. |last20=Mortier |first20=Annelies |last21=Santos |first21=Nuno C. |last22=Sousa |first22=Sérgio G. |last23=Turtelboom |first23=Emma V. |last24=Wheatley |first24=Peter J. |last25=Vanderburg |first25=Andrew M.}}</ref>

The rings of the Solar System's gas giants are aligned with their planet's equator. However, for exoplanets that orbit close to their star, tidal forces from the star would lead to the outermost rings of a planet being aligned with the planet's orbital plane around the star. A planet's innermost rings would still be aligned with the planet's equator so that if the planet has a [[axial tilt|tilted rotational axis]], then the different alignments between the inner and outer rings would create a warped ring system.<ref>{{cite journal |arxiv=1104.3863|bibcode = 2011ApJ...734..117S |doi = 10.1088/0004-637X/734/2/117 | volume=734 |issue = 2 |title=Warm Saturns: On the Nature of Rings around Extrasolar Planets That Reside inside the Ice Line |journal=The Astrophysical Journal |page=117|year = 2011 |last1 = Schlichting |first1 = Hilke E. |last2 = Chang |first2=Philip |s2cid=42698264}}</ref>