Editing Lyra (section)

===Exoplanets===
In orbit around the orange subgiant star [[HD 177830]] is one of the earliest [[exoplanet]]s to be detected. A jovian-mass planet, it orbits in an eccentric orbit with a period of 390 days.<ref name="VogtMarcy2000">{{cite journal |last1=Vogt |first1=Steven S. |last2=Marcy |first2=Geoffrey W. |last3=Butler |first3=R. Paul |last4=Apps |first4=Kevin |title=Six New Planets from the Keck Precision Velocity Survey |journal=The Astrophysical Journal |volume=536 |issue=2 |date=2000 |pages=902–914 |bibcode=2000ApJ...536..902V |doi=10.1086/308981 |arxiv=astro-ph/9911506 |s2cid=119375519 }}</ref> A second planet closer to the star was discovered in 2011.<ref name="MeschiariLaughlin2011">{{cite journal |last1=Meschiari |first1=Stefano |last2=Laughlin |first2=Gregory |last3=Vogt |first3=Steven S. |last4=Butler |first4=R. Paul |last5=Rivera |first5=Eugenio J. |last6=Haghighipour |first6=Nader |last7=Jalowiczor |first7=Peter |title=The Lick-Carnegie Survey: Four New Exoplanet Candidates |journal=The Astrophysical Journal |volume=727 |issue=2 |date=2011 |pages=117 |bibcode=2011ApJ...727..117M |doi=10.1088/0004-637X/727/2/117 |arxiv=1011.4068 |s2cid=59065004 }}</ref> Visible to the naked eye are [[HD 173416]], a [[yellow giant]] hosting a planet over twice the mass of Jupiter discovered in 2009;<ref name="LiuSato2009">{{cite journal |last1=Liu |first1=Yu-Juan |last2=Sato |first2=Bun'ei |last3=Zhao |first3=Gang |last4=Ando |first4=Hiroyasu |title=A planetary companion orbiting the intermediate-mass G Giant HD 173416 |journal=Research in Astronomy and Astrophysics |volume=9 |issue=1 |date=2009 |pages=1–4 |bibcode=2009RAA.....9....1L |doi=10.1088/1674-4527/9/1/001|s2cid=250679097 |doi-access=free }}</ref> and [[HD 176051]], a low-mass binary star containing another high-mass planet.<ref name="MuterspaughLane2010">{{cite journal |last1=Muterspaugh |first1=Matthew W. |last2=Lane |first2=Benjamin F. |last3=Kulkarni |first3=S. R. |last4=Konacki |first4=Maciej |last5=Burke |first5=Bernard F. |last6=Colavita |first6=M. M. |last7=Shao |first7=M. |last8=Hartkopf |first8=William I. |last9=Boss |first9=Alan P. |last10=Williamson |first10=M. |title=The Phases Differential Astrometry Data Archive. V. Candidate Substellar Companions to Binary Systems |journal=The Astronomical Journal |volume=140 |issue=6 |date=2010 |pages=1657–1671 |bibcode=2010AJ....140.1657M |doi=10.1088/0004-6256/140/6/1657 |arxiv=1010.4048 |s2cid=59585356 }}</ref> Just short of naked-eye visibility is [[HD 178911]], a triple system consisting of a close binary and a visually separable sunlike star. The sunlike star has a planet with over 6 Jupiter masses discovered in 2001, the second found in a triple system after that of [[16 Cygni]].<ref name="ZuckerNaef2002">{{cite journal |last1=Zucker |first1=S. |last2=Naef |first2=D. |last3=Latham |first3=D. W. |last4=Mayor |first4=M. |last5=Mazeh |first5=T. |last6=Beuzit |first6=J. L. |last7=Drukier |first7=G. |last8=Perrier-Bellet |first8=C. |last9=Queloz |first9=D. |last10=Sivan |first10=J. P. |last11=Torres |first11=G. |last12=Udry |first12=S. |title=A Planet Candidate in the Stellar Triple System HD 178911 |journal=The Astrophysical Journal |volume=568 |issue=1 |date=2002 |pages=363–368 |bibcode=2002ApJ...568..363Z |doi=10.1086/338892 |arxiv=astro-ph/0111550 |s2cid=16548934 }}</ref>

One of the most-studied exoplanets in the night sky is [[TrES-1b]], in orbit around the star [[GSC 02652-01324]]. Detected from a [[planetary transit|transit]] of its parent star, the planet has around 3/4 the mass of Jupiter, yet orbits its parent star in only three days.<ref name="AlonsoBrown2004">{{cite journal |last1=Alonso |first1=Roi |last2=Brown |first2=Timothy M. |last3=Torres |first3=Guillermo |last4=Latham |first4=David W. |last5=Sozzetti |first5=Alessandro |last6=Mandushev |first6=Georgi |last7=Belmonte |first7=Juan A. |last8=Charbonneau |first8=David |last9=Deeg |first9=Hans J. |last10=Dunham |first10=Edward W. |last11=O'Donovan |first11=Francis T. |last12=Stefanik |first12=Robert P. |title=TrES-1: The Transiting Planet of a Bright K0 V Star |journal=The Astrophysical Journal |volume=613 |issue=2 |date=2004 |pages=L153–L156 |bibcode=2004ApJ...613L.153A |doi=10.1086/425256 |arxiv=astro-ph/0408421 |s2cid=8940599 }}</ref> The transits have been reported to have anomalies multiple times. Originally thought to be possibly due to the presence of an Earth-like planet, it is now accepted that the irregularities are due to a large starspot.<ref name="DittmannClose2009">{{cite journal |last1=Dittmann |first1=Jason A. |last2=Close |first2=Laird M. |last3=Green |first3=Elizabeth M. |last4=Fenwick |first4=Mike |title=A TENTATIVE DETECTION OF A STARSPOT DURING CONSECUTIVE TRANSITS OF AN EXTRASOLAR PLANET FROM THE GROUND: NO EVIDENCE OF A DOUBLE TRANSITING PLANET SYSTEM AROUND TrES-1 |journal=The Astrophysical Journal |volume=701 |issue=1 |date=2009 |pages=756–763 |bibcode=2009ApJ...701..756D |doi=10.1088/0004-637X/701/1/756 |arxiv=0906.4320 |s2cid=16254932 }}</ref> Also discovered by the transit method is [[WASP-3b]], with 1.75 times the mass of Jupiter. At the time of its discovery, it was one of the hottest known exoplanets, in orbit around the [[F-type main-sequence star]] [[WASP-3]].<ref name="PollaccoSkillen2008">{{cite journal |last1=Pollacco |first1=D. |last2=Skillen |first2=I. |last3=Collier Cameron |first3=A. |last4=Loeillet |first4=B. |last5=Stempels |first5=H. C. |last6=Bouchy |first6=F. |last7=Gibson |first7=N. P. |last8=Hebb |first8=L. |last9=Hébrard |first9=G. |last10=Joshi |first10=Y. C. |last11=McDonald |first11=I. |last12=Smalley |first12=B. |last13=Smith |first13=A. M. S. |last14=Street |first14=R. A. |last15=Udry |first15=S. |last16=West |first16=R. G. |last17=Wilson |first17=D. M. |last18=Wheatley |first18=P. J. |last19=Aigrain |first19=S. |last20=Alsubai |first20=K. |last21=Benn |first21=C. R. |last22=Bruce |first22=V. A. |last23=Christian |first23=D. J. |last24=Clarkson |first24=W. I. |last25=Enoch |first25=B. |last26=Evans |first26=A. |last27=Fitzsimmons |first27=A. |last28=Haswell |first28=C. A. |last29=Hellier |first29=C. |last30=Hickey |first30=S. |last31=Hodgkin |first31=S. T. |last32=Horne |first32=K. |last33=Hrudková |first33=M. |last34=Irwin |first34=J. |last35=Kane |first35=S. R. |last36=Keenan |first36=F. P. |last37=Lister |first37=T. A. |last38=Maxted |first38=P. |last39=Mayor |first39=M. |last40=Moutou |first40=C. |last41=Norton |first41=A. J. |last42=Osborne |first42=J. P. |last43=Parley |first43=N. |last44=Pont |first44=F. |last45=Queloz |first45=D. |last46=Ryans |first46=R. |last47=Simpson |first47=E. |title=WASP-3b: a strongly irradiated transiting gas-giant planet |journal=Monthly Notices of the Royal Astronomical Society |volume=385 |issue=3 |date=2008 |pages=1576–1584 |bibcode=2008MNRAS.385.1576P |doi=10.1111/j.1365-2966.2008.12939.x |doi-access=free |arxiv=0711.0126 |s2cid=2317308 }}</ref> Similar to TrES-1b, irregularities in the transits had left open the possibility of a second planet, although this now appears unlikely as well.<ref name="MaciejewskiNiedzielski2013">{{cite journal |last1=Maciejewski |first1=G. |last2=Niedzielski |first2=A. |last3=Wolszczan |first3=A. |last4=Nowak |first4=G. |last5=Neuhäuser |first5=R. |last6=Winn |first6=J. N. |last7=Deka |first7=B. |last8=Adamów |first8=M. |last9=Górecka |first9=M. |last10=Fernández |first10=M. |last11=Aceituno |first11=F. J. |last12=Ohlert |first12=J. |last13=Errmann |first13=R. |last14=Seeliger |first14=M. |last15=Dimitrov |first15=D. |last16=Latham |first16=D. W. |last17=Esquerdo |first17=G. A. |last18=McKnight |first18=L. |last19=Holman |first19=M. J. |last20=Jensen |first20=E. L. N. |last21=Kramm |first21=U. |last22=Pribulla |first22=T. |last23=Raetz |first23=St. |last24=Schmidt |first24=T. O. B. |last25=Ginski |first25=Ch. |last26=Mottola |first26=S. |last27=Hellmich |first27=S. |last28=Adam |first28=Ch. |last29=Gilbert |first29=H. |last30=Mugrauer |first30=M. |last31=Saral |first31=G. |last32=Popov |first32=V. |last33=Raetz |first33=M. |title=Constraints on a Second Planet in the Wasp-3 System |journal=The Astronomical Journal |volume=146 |issue=6 |date=2013 |pages=147 |bibcode=2013AJ....146..147M |doi=10.1088/0004-6256/146/6/147 |arxiv=1309.6733 |s2cid=17255900 }}</ref>

Lyra is one of three constellations (along with neighboring Cygnus and Draco) to be in the [[Kepler Mission]]'s field of view, and as such it contains many more known exoplanets than most constellations. One of the first discovered by the mission is [[Kepler-7b]], an extremely low-density exoplanet with less than half the mass of Jupiter, yet nearly 1.5 times the radius.<ref name="LathamBorucki2010">{{cite journal |last1=Latham |first1=David W. |last2=Borucki |first2=William J. |last3=Koch |first3=David G. |last4=Brown |first4=Timothy M. |last5=Buchhave |first5=Lars A. |last6=Basri |first6=Gibor |last7=Batalha |first7=Natalie M. |last8=Caldwell |first8=Douglas A. |last9=Cochran |first9=William D. |last10=Dunham |first10=Edward W. |last11=Fűrész |first11=Gabor |last12=Gautier |first12=Thomas N. |last13=Geary |first13=John C. |last14=Gilliland |first14=Ronald L. |last15=Howell |first15=Steve B. |last16=Jenkins |first16=Jon M. |last17=Lissauer |first17=Jack J. |last18=Marcy |first18=Geoffrey W. |last19=Monet |first19=David G. |last20=Rowe |first20=Jason F. |last21=Sasselov |first21=Dimitar D. |title=KEPLER-7b: A TRANSITING PLANET WITH UNUSUALLY LOW DENSITY |journal=The Astrophysical Journal |volume=713 |issue=2 |date=2010 |pages=L140–L144 |bibcode=2010ApJ...713L.140L |doi=10.1088/2041-8205/713/2/L140 |arxiv=1001.0190 |s2cid=55061694 }}</ref> Almost as sparse is [[Kepler-8b]], only slightly more massive and of a similar radius.<ref name="JenkinsBorucki2010">{{cite journal |last1=Jenkins |first1=Jon M. |last2=Borucki |first2=William J. |last3=Koch |first3=David G. |last4=Marcy |first4=Geoffrey W. |last5=Cochran |first5=William D. |last6=Welsh |first6=William F. |last7=Basri |first7=Gibor |last8=Batalha |first8=Natalie M. |last9=Buchhave |first9=Lars A. |last10=Brown |first10=Timothy M. |last11=Caldwell |first11=Douglas A. |last12=Dunham |first12=Edward W. |last13=Endl |first13=Michael |last14=Fischer |first14=Debra A. |last15=Gautier |first15=Thomas N. |last16=Geary |first16=John C. |last17=Gilliland |first17=Ronald L. |last18=Howell |first18=Steve B. |last19=Isaacson |first19=Howard |last20=Johnson |first20=John Asher |last21=Latham |first21=David W. |last22=Lissauer |first22=Jack J. |last23=Monet |first23=David G. |last24=Rowe |first24=Jason F. |last25=Sasselov |first25=Dimitar D. |last26=Howard |first26=Andrew W. |last27=MacQueen |first27=Phillip |last28=Orosz |first28=Jerome A. |last29=Chandrasekaran |first29=Hema |last30=Twicken |first30=Joseph D. |last31=Bryson |first31=Stephen T. |last32=Quintana |first32=Elisa V. |last33=Clarke |first33=Bruce D. |last34=Li |first34=Jie |last35=Allen |first35=Christopher |last36=Tenenbaum |first36=Peter |last37=Wu |first37=Hayley |last38=Meibom |first38=Søren |last39=Klaus |first39=Todd C. |last40=Middour |first40=Christopher K. |last41=Cote |first41=Miles T. |last42=McCauliff |first42=Sean |last43=Girouard |first43=Forrest R. |last44=Gunter |first44=Jay P. |last45=Wohler |first45=Bill |last46=Hall |first46=Jennifer R. |last47=Ibrahim |first47=Khadeejah |last48=Kamal Uddin |first48=AKM |last49=Wu |first49=Michael S. |last50=Bhavsar |first50=Paresh A. |last51=Van Cleve |first51=Jeffrey |last52=Pletcher |first52=David L. |last53=Dotson |first53=Jessie L. |last54=Haas |first54=Michael R. |title=DISCOVERY AND ROSSITER-McLAUGHLIN EFFECT OF EXOPLANET KEPLER-8b |journal=The Astrophysical Journal |volume=724 |issue=2 |date=2010 |pages=1108–1119 |bibcode=2010ApJ...724.1108J |doi=10.1088/0004-637X/724/2/1108 |arxiv=1001.0416 |s2cid=13181333 }}</ref> The [[Kepler-20]] system contains five known planets; three of them are only slightly smaller than [[Neptune]],<ref name="GautierCharbonneau2012">{{cite journal |last1=Gautier |first1=Thomas N. |last2=Charbonneau |first2=David |last3=Rowe |first3=Jason F. |last4=Marcy |first4=Geoffrey W. |last5=Isaacson |first5=Howard |last6=Torres |first6=Guillermo |last7=Fressin |first7=Francois |last8=Rogers |first8=Leslie A. |last9=Désert |first9=Jean-Michel |last10=Buchhave |first10=Lars A. |last11=Latham |first11=David W. |last12=Quinn |first12=Samuel N. |last13=Ciardi |first13=David R. |last14=Fabrycky |first14=Daniel C. |last15=Ford |first15=Eric B. |last16=Gilliland |first16=Ronald L. |last17=Walkowicz |first17=Lucianne M. |author17-link=Lucianne Walkowicz |last18=Bryson |first18=Stephen T. |last19=Cochran |first19=William D. |last20=Endl |first20=Michael |last21=Fischer |first21=Debra A. |last22=Howell |first22=Steve B. |last23=Horch |first23=Elliott P. |last24=Barclay |first24=Thomas |last25=Batalha |first25=Natalie |last26=Borucki |first26=William J. |last27=Christiansen |first27=Jessie L. |last28=Geary |first28=John C. |last29=Henze |first29=Christopher E. |last30=Holman |first30=Matthew J. |last31=Ibrahim |first31=Khadeejah |last32=Jenkins |first32=Jon M. |last33=Kinemuchi |first33=Karen |last34=Koch |first34=David G. |last35=Lissauer |first35=Jack J. |last36=Sanderfer |first36=Dwight T. |last37=Sasselov |first37=Dimitar D. |last38=Seager |first38=Sara |last39=Silverio |first39=Kathryn |last40=Smith |first40=Jeffrey C. |last41=Still |first41=Martin |last42=Stumpe |first42=Martin C. |last43=Tenenbaum |first43=Peter |last44=Van Cleve |first44=Jeffrey |title=Kepler-20: A Sun-Like Star with Three Sub-Neptune Exoplanets and Two Earth-Size Candidates |journal=The Astrophysical Journal |volume=749 |issue=1 |date=2012 |pages=15 |bibcode=2012ApJ...749...15G |doi=10.1088/0004-637X/749/1/15 |arxiv=1112.4514 |s2cid=18765025 }}</ref> while the other two are some of the first [[Earth]]-sized exoplanets to be discovered.<ref name="FressinTorres2011">{{cite journal |last1=Fressin |first1=Francois |last2=Torres |first2=Guillermo |last3=Rowe |first3=Jason F. |last4=Charbonneau |first4=David |last5=Rogers |first5=Leslie A. |last6=Ballard |first6=Sarah |last7=Batalha |first7=Natalie M. |last8=Borucki |first8=William J. |last9=Bryson |first9=Stephen T. |last10=Buchhave |first10=Lars A. |last11=Ciardi |first11=David R. |last12=Désert |first12=Jean-Michel |last13=Dressing |first13=Courtney D. |last14=Fabrycky |first14=Daniel C. |last15=Ford |first15=Eric B. |last16=Gautier III |first16=Thomas N. |last17=Henze |first17=Christopher E. |last18=Holman |first18=Matthew J. |last19=Howard |first19=Andrew |last20=Howell |first20=Steve B. |last21=Jenkins |first21=Jon M. |last22=Koch |first22=David G. |last23=Latham |first23=David W. |last24=Lissauer |first24=Jack J. |last25=Marcy |first25=Geoffrey W. |last26=Quinn |first26=Samuel N. |last27=Ragozzine |first27=Darin |last28=Sasselov |first28=Dimitar D. |last29=Seager |first29=Sara |last30=Barclay |first30=Thomas |last31=Mullally |first31=Fergal |last32=Seader |first32=Shawn E. |last33=Still |first33=Martin |last34=Twicken |first34=Joseph D. |last35=Thompson |first35=Susan E. |last36=Uddin |first36=Kamal |title=Two Earth-sized planets orbiting Kepler-20 |journal=Nature |volume=482 |issue=7384 |date=2011 |pages=195–198 |bibcode=2012Natur.482..195F |doi=10.1038/nature10780 |arxiv=1112.4550 |pmid=22186831|s2cid=3182266 }}</ref> [[Kepler-37]] is another star with an exoplanet discovered by Kepler; the planet is the smallest known [[extrasolar planet]] known as of February 2013.

In April 2013, it was announced that of the five planets orbiting [[Kepler-62]], at least two—[[Kepler-62e]] and [[Kepler-62f]]—are within the boundaries of the [[habitable zone]] of that star, where scientists think liquid water could exist, and are both candidates for being a solid, rocky, earth-like planet.<ref name = "BoruckiKepler-62">{{Cite journal | last=Borucki | first=William J. | author-link=William J. Borucki | display-authors=etal | title=Kepler-62: A Five-Planet System with Planets of 1.4 and 1.6 Earth Radii in the Habitable Zone | journal=Science Express | date=18 April 2013 | doi=10.1126/science.1234702 | access-date=18 March 2022 | url=https://www.science.org/doi/10.1126/science.1234702 | arxiv=1304.7387 | bibcode=2013Sci...340..587B | pmid=23599262 | volume=340 | issue=6132 | pages=587–90 | hdl=1721.1/89668 | s2cid=21029755 | archive-date=2 May 2022 | archive-url=https://web.archive.org/web/20220502115940/https://www.science.org/doi/10.1126/science.1234702 | url-status=live }}</ref><ref name="NASA-20130418">{{cite web |last1=Johnson |first1=Michele |last2=Harrington |first2=J.D. |title=NASA's Kepler Discovers Its Smallest 'Habitable Zone' Planets to Date |url=http://www.nasa.gov/mission_pages/kepler/news/kepler-62-kepler-69.html |date=18 April 2013 |work=[[NASA]] |access-date=18 March 2022 |archive-date=8 May 2020 |archive-url=https://web.archive.org/web/20200508010029/https://www.nasa.gov/mission_pages/kepler/news/kepler-62-kepler-69.html |url-status=dead }}</ref> The [[exoplanet]]s are 1.6 and 1.4 times the diameter of [[Earth]] respectively,<ref name = "BoruckiKepler-62" /> with their star [[Kepler-62]] at a distance of 1,200 light-years.<ref>{{cite news |last=Grant |first=Andrew |title=Most Earthlike planets yet seen bring Kepler closer to its holy grail |url=http://www.sciencenews.org/view/generic/id/349783/description/Most_Earthlike_planets_yet_seen_bring_Kepler_closer_to_its_holy_grail |access-date=19 April 2013 |newspaper=ScienceNews.org |date=18 April 2013 |archive-date=21 April 2013 |archive-url=https://web.archive.org/web/20130421071835/http://www.sciencenews.org/view/generic/id/349783/description/Most_Earthlike_planets_yet_seen_bring_Kepler_closer_to_its_holy_grail |url-status=live }}</ref>