WASP-12b (ekzosayyora) sahifasining manbasini koʻrish

{{Sayyora bilgiqutisi|tasvir=Exoplanet Comparison WASP-12 b.png|izoh=WASP-12b ni (o'ngda) Yupiter bilan taqqoslash
<!-- DISCOVERY           -->|apsis=astron|discoverer=Cameron ([[SuperWASP]])|discovery_site=[[SAAO]]|period=1.091423 ± 3e-6 [[day]]s|mean_radius=1.900{{±|0.057|0.055}},<ref name=collins>{{Cite journal|bibcode=2017AJ....153...78C|title=Transit Timing Variation Measurements of WASP-12b and Qatar-1b: No Evidence for Additional Planets|last1=Collins|first1=Karen A|last2=Kielkopf|first2=John F|last3=Stassun|first3=Keivan G|journal=The Astronomical Journal|year=2017|volume=153|issue=2|page=78|doi=10.3847/1538-3881/153/2/78|arxiv=1512.00464|s2cid=55191644}}</ref> {{Jupiter radius|link=y}}|density={{convert|266|kg/m3|lk=on|abbr=on}}<ref name=collins />|name=WASP-12b|discovered=2008-yil, 1-aprel<ref name=wasp />|discovery_method=Tranzit
<!-- DESIGNATIONS        -->
<!-- ORBITAL             -->|semimajor={{val|0.0234|0.00056|0.00050|u=AU}}|eccentricity=0.049 ± 0.015|inclination={{val|83.37|0.72|0.64|u=°}}|arg_peri={{val|83.37|0.72|0.64|u=°}}|star=[[WASP-12]]
<!-- PHYS CHARS          -->|mass={{val|1.47|0.076|0.069}}<ref name=collins /> {{Jupiter mass|link=y}}|surface_grav={{val|3.004|0.015}} [[g-force|g]]<ref name=collins />|single_temperature={{val|3128|64|68|u=K}} ({{val|2885|64|68|u=°C}}, {{val|5225|147|155|u=°F}})<ref>{{citation|arxiv=2102.00052|title=Phase curve and variability analysis of WASP-12b using TESS photometry|year=2021|doi=10.1093/mnrasl/slab014|last1=Owens|first1=Niall|last2=De Mooij|first2=E J W.|last3=Watson|first3=C. A.|last4=Hooton|first4=M. J.|journal=Monthly Notices of the Royal Astronomical Society: Letters|volume=503|pages=L38–L46}}</ref>
<!-- ATMOSPHERE          -->
<!-- NOTES               -->}}'''WASP-12b''' — WASP-12 [[Yulduz|yulduzi]] atrofida aylanib yuruvchi qaynoq Yupiter sinfiga kiruvchi ekzosayyora.<ref>{{Veb manbasi|muallif=Starr|ism=Michelle|sarlavha=Astronomers Just Found a 'Hot Jupiter' So Dark, It Absorbs Nearly 99% of Light|url=https://www.sciencealert.com/hot-jupiter-wasp-104b-one-of-the-darkest-planets-ever|ish=ScienceAlert}}</ref> (quyoshdan tashqari [[Ekzosayyora|sayyoralar]] sinfi). SuperWASP sayyoralar tranzit tadqiqoti tomonidan 2008-yil 1-aprelda kashf etilgan.<ref name="wasp">{{Veb manbasi|url=http://wasp-planets.net/wasp-planets/|sarlavha=WASP Planets|ish=SuperWASP|sana=December 5, 2013|kirish sanasi=2016-01-26}}</ref> Sayyora oʻz yulduzini aylanib chiqishi uchun bor-yoʻgʻi bir Yer kunidan sal koʻproq vaqt ketadi, [[Yer|Yerning]] [[Quyosh]] atrofida aylanishi uchun 365,25 kundan farqli oʻlaroq, uning oʻz yulduzidan uzoqligi (taxminan faqat <math>\textstyle\frac{1}{43}</math> Yerning Quyoshdan uzoqligi va ekssentrikligi [[Yupiter|Yupiternikiga]] teng. Binobarin, u ekzosayyoralar uchun eng past zichliklardan biriga ega (yulduzdan energiya oqimi bilan „shishirilgan“). 2013-yil 3-dekabr kuni [[Hubble kosmik teleskopi]] (HST) bilan ishlaydigan olimlar [[ekzosayyora]] atmosferasida [[suv]] aniqlangani haqida xabar berishdi.<ref name="NASA-20131203">{{Veb manbasi|muallif=Staff|sarlavha=Hubble Traces Subtle Signals of Water on Hazy Worlds|url=http://www.nasa.gov/content/goddard/hubble-traces-subtle-signals-of-water-on-hazy-worlds/|nashriyot=[[NASA]]|sana=3 December 2013|kirish sanasi=4 December 2013}}</ref><ref name="ApJ-20131203">{{Cite journal|last=Mandell|first1=Avi M.|last2=Haynes|first2=Korey|last3=Sinukoff|first3=Evan|last4=Madhusudhan|first4=Nikku|last5=Burrows|first5=Adam|last6=Deming|first6=Drake|title=Exoplanet Transit Spectroscopy Using WFC3: WASP-12 b, WASP-17 b, and WASP-19 b|date=3 December 2013|journal=[[Astrophysical Journal]]|volume=779|issue=2|page=128|doi=10.1088/0004-637X/779/2/128|arxiv=1310.2949|bibcode=2013ApJ...779..128M}}</ref> 2014-yil iyul oyida NASA quyoshga oʻxshash yulduzlar atrofida aylanib yuruvchi uchta ekzosayyorada (HD 189733b, HD 209458b, WASP-12b) juda quruq [[Ekzosayyora|atmosfera]] topilganini eʼlon qildi.<ref name="NASA-20140724">{{Veb manbasi|muallif=Harrington|ism=J.D.|sarlavha=RELEASE 14-197 - Hubble Finds Three Surprisingly Dry Exoplanets|url=http://www.nasa.gov/press/2014/july/hubble-finds-three-surprisingly-dry-exoplanets/|sana=July 24, 2014|ish=[[NASA]]|kirish sanasi=July 25, 2014}}</ref>

2017-yil sentabrida HST ustida ishlayotgan tadqiqotchilar WASP-12b uning yuzasida porlayotgan yorug‘likning atigi 6 foizini aks ettirishini eʼlon qilishdi. Natijada ekzosayyora „asfaltdek qora“ va „qop qora“ deb taʼriflangan.<ref>{{Yangiliklar manbasi |last=Wall |first=Mike |date=18 September 2017 |title=The hellish world WASP-12b is darker than fresh asphalt in visible light, but glows red-hot in infrared |work=[[Scientific American]] |url=https://www.scientificamerican.com/article/astronomers-discover-pitch-black-exoplanet/ |access-date=19 September 2017}}</ref>

== Xususiyatlari ==
[[Fayl:The_Pitch-Black_Exoplanet_WASP-12b.jpg|link=//upload.wikimedia.org/wikipedia/commons/thumb/8/80/The_Pitch-Black_Exoplanet_WASP-12b.jpg/200px-The_Pitch-Black_Exoplanet_WASP-12b.jpg|left|thumb|200x200px| WASP-12b oʻz yuzasida porlayotgan yorugʻlikning 94 % ni oʻzlashtiradi. Bu juda past [[Albedo|albedoga]] olib keladi.<ref>{{Veb manbasi|sarlavha=Hubble observes pitch black planet|url=https://www.spacetelescope.org/news/heic1714/|ish=www.spacetelescope.org|kirish sanasi=15 September 2017}}</ref>]]
Qaynoq Yupiter ekzosayyoralari toʻlqinlarning oʻzaro taʼsiri bilan „qulflangan faza“ boʻlgani uchun (yaʼni, xuddi shu tomoni har doim yulduzga qaraydi, xuddi Oyning bir tomoni doimo Yerga qaragandek)..Buning natijasida sayyora atmosferasi atrofida juda kuchli shamollar esib turadi, deb taxmin qilinadi.Taylor Bell va Nicolas Cowan [[Vodorod|vodorodning]] kunlik ionlashuvga moyil boʻlishini taʼkidladilar. Shamolda sovuqroq yuzaga oqib oʻtgandan soʻng, u neytral atomlarga qayta birlashishga moyil boʻladi va shu bilan issiqlikni tashishni kuchaytiradi.Sayyora oʻz yulduziga shunchalik yaqinki, uning toʻlqin kuchlari uni [[Ellipsoid|tuxum shakliga keltirmoqda]] va yiliga taxminan 10 <sup>−7 MJ</sup> M yoki taxminan 189 kvadrillion tonna) atmosferasini tortib oladi.<ref>{{Cite journal|first1=Shu-lin|last=Li|first2=N.|last2=Miller|first3=Douglas N. C.|last3=Lin|first4=Jonathan J.|last4=Fortney|date=2010|title=WASP-12b as a prolate, inflated and disrupting planet from tidal dissipation|journal=[[Nature (journal)|Nature]]|volume=463|issue=7284|pages=1054–1056|doi=10.1038/nature08715|pmid=20182506|bibcode=2010Natur.463.1054L|arxiv=1002.4608}}</ref> „Toʻlqinli issiqlik“ va sayyoraning uning yulduziga yaqinligi birlashtirilib, sirt harorati {{Convert|2500|K|°C|-2}} dan oshadi.

2010-yil 20-may kuni [[Hubble kosmik teleskopi]] WASP-12b o‘z yulduzi tomonidan „yutib yuborilayotgani“ aniqladi. Olimlar yulduzlar sayyoralarni yutib yuborishi mumkinligini bilishgan. Ammo bunday hodisa birinchi marta bunchalik aniq kuzatilgan edi. NASAning hisob-kitoblariga ko‘ra, sayyoraning umri tugashiga 10 million yil qolgan.<ref name="Hubble observation">[http://www.nasa.gov/mission_pages/hubble/science/planet-eater.html Hubble Finds a Star Eating a Planet] {{Webarxiv|url=https://web.archive.org/web/20211111124425/http://www.nasa.gov/mission_pages/hubble/science/planet-eater.html |date=2021-11-11 }} nasa.gov. 2010-05-20. Retrieved on 2010-12-10.</ref>

Hubble teleskopi oʻzining Kosmik kelib chiqishi spektrografi (COS) yordamida sayyorani kuzatdi. Kuzatishlar Pekin universiteti professori Shu-Lin Li tomonidan 2009-yil fevral oyida ''Nature'' jurnalida chop etilgan bashoratlarni tasdiqladi. Sayyora atmosferasi Yupiterning radiusidan deyarli uch baravar katta boʻlib, sayyoraning oʻzi esa Yupiterdan 40 % koʻproq [[Massa|massaga]] ega.

== Orbitasi ==
2012-yilda Rossiter-McLaughlin effektidan foydalangan holda oʻtkazilgan tadqiqotda, WASP-12b orbitasi oʻz yulduzining ekvator tekisligi bilan 59 +15 ga juda notoʻgʻri ekanligini aniqladi.+15<nowiki></br></nowiki> − 20 °.<ref>{{Citation|arxiv=1206.6105|title=Obliquities of Hot Jupiter host stars: Evidence for tidal interactions and primordial misalignments|year=2012|doi=10.1088/0004-637X/757/1/18|last=Albrecht|first1=Simon|last2=Winn|first2=Joshua N.|last3=Johnson|first3=John A.|last4=Howard|first4=Andrew W.|last5=Marcy|first5=Geoffrey W.|last6=Butler|first6=R. Paul|last7=Arriagada|first7=Pamela|last8=Crane|first8=Jeffrey D.|last9=Shectman|first9=Stephen A.|journal=The Astrophysical Journal|volume=757|issue=1|page=18|bibcode=2012ApJ...757...18A}}</ref>

2019-yildagi tadqiqot shuni koʻrsatdiki, ikki tranzit oʻrtasidagi vaqt oraligʻi 2008-yilda kashf etilganidan beri yiliga 29 ± 2 ms sekundga qisqardi. Qiymat 2020-yilda 32,53 ± msek /yilga yangilandi. Bu WASP-12b ning taxminiy umrini 2,90 ± million yilni tashkil etdi.<ref>{{Citation|arxiv=2012.02211|title=Decaying Orbit of the Hot Jupiter WASP-12b: Confirmation with TESS Observations|year=2021|last=Turner|first1=Jake D.|last2=Ridden-Harper|first2=Andrew|last3=Jayawardhana|first3=Ray|journal=The Astronomical Journal|volume=161|issue=2|page=72|doi=10.3847/1538-3881/abd178|bibcode=2021AJ....161...72T}}</ref> Tadqiqot shuni koʻrsatdiki, WASP-12b orbitasi sayyora va WASP-12 yulduzi oʻrtasidagi toʻlqinli oʻzaro taʼsirlar natijasida parchalanadi. Ushbu parchalanish tufayli orbital davr qisqaradi va sayyora yulduzning bir qismiga aylanmaguncha oʻz yulduziga yaqinlashadi. Yemirilish WASP-19b ning parchalanishidan ancha tezroq boʻlib, bu joriy maʼlumotlar bilan parchalanishni koʻrsatmaydi.<ref>{{Veb manbasi|url=https://wasp-planets.net/2019/11/26/the-orbit-of-wasp-12b-is-decaying/|sarlavha=The orbit of WASP-12b is decaying|muallif=waspplanets|sana=2019-11-26|ish=WASP Planets|til=en|kirish sanasi=2020-01-01}}</ref><ref>{{Cite journal|last=Yee|first1=Samuel W.|last2=Winn|first2=Joshua N.|last3=Knutson|first3=Heather A.|last4=Patra|first4=Kishore C.|last5=Vissapragada|first5=Shreyas|last6=Zhang|first6=Michael M.|last7=Holman|first7=Matthew J.|last8=Shporer|first8=Avi|last9=Wright|first9=Jason T.|date=2019-11-20|title=The Orbit of WASP-12b is Decaying|journal=The Astrophysical Journal|volume=888|pages=L5|arxiv=1911.09131|doi=10.3847/2041-8213/ab5c16}}</ref> 2022-yilda parchalanish tezligi yiliga 29,81 ± msek.gachaligi aniqlandi.<ref>{{Cite journal|last=Wong|first1=Ian|last2=Shporer|first2=Avi|last3=Vissapragada|first3=Shreyas|last4=Greklek-McKeon|first4=Michael|last5=Knutson|first5=Heather A.|last6=Winn|first6=Joshua N.|last7=Benneke|first7=Björn|title=TESS Revisits WASP-12: Updated Orbital Decay Rate and Constraints on Atmospheric Variability|journal=The Astronomical Journal|date=20 January 2022|volume=163|issue=4|page=175|doi=10.3847/1538-3881/ac5680|arxiv=2201.08370|bibcode=2022AJ....163..175W}}</ref>

=== Uglerod tarkibi ===
2010-yilda oʻtkazilgan tadqiqotda eʼlon qilingan dalillar shuni koʻrsatadiki, WASP-12b [[Uglerod|uglerodning]] [[Kislorod|kislorodga]] nisbati yaxshilangan. Bu Quyoshnikidan sezilarli darajada yuqori, bu esa u uglerodga boy gaz giganti ekanligini koʻrsatadi. Kuzatishlar bilan mos keladigan C/O nisbati taxminan 1 ga teng. Quyosh qiymati esa 0,54 ni tashkil qiladi. C/O nisbatlari yulduz tizimida uglerodga boy sayyoralar paydo boʻlgan boʻlishi mumkinligini koʻrsatadi.<ref name="C-O-ratio">{{Cite journal|last=Madhusudhan|first1=N.|last2=Harrington|first2=J.|last3=Stevenson|first3=K. B.|last4=Nymeyer|first4=S.|last5=Campo|first5=C. J.|last6=Wheatley|first6=P. J.|last7=Deming|first7=D.|last8=Blecic|first8=J.|last9=Hardy|first9=R. A.|doi=10.1038/nature09602|title=A high C/O ratio and weak thermal inversion in the atmosphere of exoplanet WASP-12b|journal=Nature|volume=469|issue=7328|pages=64–67|year=2010|pmid=21150901|bibcode=2011Natur.469...64M|arxiv=1012.1603}}</ref> Ushbu tadqiqot ortidagi tadqiqotchilardan biri „kisloroddan koʻra koʻproq uglerod bilan siz [[olmos]] yoki [[grafit]] kabi sof uglerodli jinslarni olasiz“ deb izoh berdi.

Nashr etilgan tadqiqotda aytilishicha, „WASP-12b kabi uglerodga boy gigant sayyoralar kuzatilmagan boʻlsa-da, nazariya uglerod ustunligidagi qattiq sayyoralar uchun son-sanoqsiz kompozitsiyalarni bashorat qilmoqda. Masalan, yer yuzidagi oʻlchamdagi uglerod sayyoralarida, Yerning silikat tarkibidan farqli oʻlaroq, grafit yoki olmosli qatlamlar hukmron boʻlishi mumkin.“<ref name="C-O-ratio"/> Bu soʻzlar OAVda katta yangilik sifatida qabul qilindi.<ref>{{Yangiliklar manbasi |last=Lorianna De Giorgio |date=10 December 2010 |title=Carbon-rich planet could house diamonds |work=[[Toronto Star]] |url=https://www.thestar.com/article/905303--carbon-rich-planet-could-house-diamonds}}</ref> Baʼzilar hatto WASP-12b ni „olmos sayyora“ deb atashdi.<ref>{{Yangiliklar manbasi |date=9 December 2010 |title=Diamond planet found by Keele University astronomers |work=[[BBC News Online]] |url=http://news.bbc.co.uk/local/stoke/hi/people_and_places/nature/newsid_9272000/9272801.stm}}</ref>

Sayyoradagi uglerod miqdori uning atmosferasida [[Is gazi|uglerod oksidi]] va [[metan]] shaklida joylashgan. Tadqiqot ''Nature'' jurnalida chop etilgan.<ref>{{Yangiliklar manbasi |last=Intagliata |first=Christopher |date=December 9, 2010 |title=Exoplanet Strikes Carbon Pay Dirt |work=[[Scientific American]] |url=http://www.scientificamerican.com/podcast/episode.cfm?id=exoplanet-strikes-carbon-paydirt-10-12-09}}</ref><gallery>
Fayl:WASP-12b (NASA).jpg|alt=WASP-12b and its host star, WASP-12 (artist conception).|WASP-12b va uning yulduzi.
Fayl:WASP-12b a Hot, Carbon-Rich Planet.jpg|alt=Hot, carbon-rich planet WASP-12b and its host star. (Exoplanet color was unknown at the time of this artist conception).|Issiq, uglerodga boy sayyora WASP-12b va uning yulduzi. (Ushbu rasm kontseptsiyasi ishlanganida ekzosayyoraning rangi noma'lum edi).
Fayl:WASP-12b.jpg|alt=WASP-12b and its host star, WASP-12 − with IR spectra noting the presence of various chemical molecules.|WASP-12b va uning asosiy yulduzi. WASP-12 - turli xil kimyoviy molekulalarning mavjudligini ko'rsatadigan [[Infrared spectroscopy|IQ spektrlari]] bilan.
Fayl:Clear to cloudy hot Jupiters.jpg|alt=Comparison of "hot Jupiter" exoplanets - from top left to lower right: WASP-12b, WASP-6b, WASP-31b, WASP-39b, HD 189733b, HAT-P-12b, WASP-17b, WASP-19b, HAT-P-1b and HD 209458b.|" [[Hot Jupiter|Qaynoq Yupiter]] " ekzosayyoralarini taqqoslash - yuqoridan chapdan pastki o'ngga: WASP-12b, [[WASP-6b]], [[WASP-31b]], [[WASP-39b|WASP-]] 39b, [[HD 189733b]], [[HAT-P-12b]], [[WASP-17b]], [[WASP-19b]], [[HAT-P-1b|HAT- P-1b]] va [[HD 209458b]] .
</gallery>

== Sunʼiy yoʻldoshi ==
Sayyora porlashining oʻzgarishi egri chizigʻini oʻrganayotgan rus astronomlari, WASP-12b orbitasida kamida bitta ekzomun atrofidagi plazma torusidan kelib chiqadigan yorugʻlikning muntazam oʻzgarishini kuzatdilar.<ref>[http://www.ria.ru/science/20120206/558647431.html Rossiyskie astronomi vpervie otkrili lunu vozle ekzoplaneti] (in Russian) — „Studying of a curve of change of shine of WASP-12b has brought to the Russian astronomers unusual result: regular splashes were found out.<...> Though stains on a star surface also can cause similar changes of shine, observable splashes are very similar on duration, a profile and amplitude that testifies for benefit of exomoon existence.“</ref> Bu kutilmaydi, chunki issiq Yupiter tipidagi sayyoralar geologik jihatdan qisqa vaqt ichida katta yoʻldoshlarini yoʻqotishi kutilmoqda.<ref>{{Cite journal|bibcode=2002ApJ...575.1087B|title=Stability of Satellites around Close-in Extrasolar Giant Planets|url=https://archive.org/details/sim_astrophysical-journal_2002-08-20_575_2/page/n510|journal=The Astrophysical Journal|volume=575|issue=2|pages=1087–1093|year=2002|last=Barnes|first1=Jason W.|last2=O'Brien|first2=D. P.|doi=10.1086/341477|arxiv=astro-ph/0205035}}</ref> Ushbu sunʼiy yoʻldosh oʻrniga [[Troyaliklar|troyan tanasi]] boʻlishi mumkin.<ref>{{Citation|arxiv=1605.02507|title=On the ultraviolet anomalies of the WASP-12 and HD 189733 systems: Trojan satellites as a plasma source|year=2016|doi=10.1093/mnras/stw1110|last=Kislyakova|first1=K. G.|last2=Pilat-Lohinger|first2=E.|last3=Funk|first3=B.|last4=Lammer|first4=H.|last5=Fossati|first5=L.|last6=Eggl|first6=S.|last7=Schwarz|first7=R.|last8=Boudjada|first8=M. Y.|last9=Erkaev|first9=N. V.|journal=Monthly Notices of the Royal Astronomical Society|volume=461|issue=1|pages=988–999|bibcode=2016MNRAS.461..988K}}</ref>

== Yana qarang ==

* TrES-2b, yorugʻlikning 90 % dan ortigʻini oʻzlashtiradigan boshqa bir sayyora.
* BPM 37093, uglerodga boy yulduz.
* SuperWASP

== Foydalanilgan adabiyotlar ==
{{Manbalar}}

== Havolalar ==

* [http://wasp-planets.net/wasp-planets/ SuperWASP Wide Angle Search for Planets: The Planets], SuperWASP.
* [https://www.newscientist.com/article/dn14943-starhugging-planet-is-hottest-and-fastest-found.html?DCMP=ILC-hmts&nsref=news2_head_dn14943 Star-hugging planet is hottest and fastest found], New Scientist.
* [http://news.bbc.co.uk/1/hi/science_and_environment/10136415.stm BBC News — Hubble spots a planet-eating star]
* [http://www.perseus.gr/Astro-Photometry-WASP-12-20110114.htm WASP-12b in transit (lightcurve)]
[[Turkum:Qaynoq Yupiter]]
[[Turkum:Ekzosayyoralarni nomlash]]
[[Turkum:Ekzosayyora]]
[[Turkum:Auriga (yulduz turkumidagi)]]