1230:
1236:
557:
1403:
1171:
1823:
1917:
1224:
1906:
463:
522:. This data was used to derive HAT-P-33's radial velocity. A far greater number of spectra were gathered for HAT-P-33 than the number usually gathered for planetary candidates to compensate for the data's jitter effect. It was concluded that the jitter in the data was caused by stellar activity and not the presence of other planets.
713:
planet's defined characteristics are based on the assumption that HAT-P-33b has an elliptical orbit, although the planet's discoverers have also derived HAT-P-33b's characteristics on the assumption that the planet has a circular orbit. The elliptical model has been chosen because it is considered to be the most likely scenario.
408:, which lies 1,310 light years away from Earth. Its discovery was reported in June 2011, although it was suspected to be a planet as early as 2004. The planet is about three-fourths the mass of Jupiter, but is almost eighty percent larger than Jupiter is; this inflation has, as with the discovery of similar planets
712:
The best fit for the shape of HAT-P-33b's orbit suggests that the orbit is slightly elliptical, as the planet's orbital eccentricity is fit to 0.148. However, because the star HAT-P-33 has such a high level of jitter, it is difficult to constrain the planet's eccentricity with accuracy. Most of the
665:
Because high levels of jitter have been detected in the spectrum of HAT-P-33, the ability to collect the most sensitive radial velocity measurements possible has been dulled. The loss of accuracy has prevented astronomers from disregarding the possibility that HAT-P-33 is actually a binary star,
510:
was used to observe the star. The resulting data invited the possibility that radial velocity measurements, which can exhibit anomalies that often indicate the presence of a planet, may have been because of background distortion (and not a planet). This possibility significantly complicated the
666:
where the secondary, dimmer companion is visually indistinguishable from the brighter primary companion. If this is the case, then the dimmer star in the HAT-P-33 system would have to have a mass that is less than 0.55 times that of the Sun. A search for a binary companion star using
552:
in the background. The possibility that HAT-P-33 is actually a binary star whose secondary companion is too dim to be distinguishable from the brighter star could not be ruled out. However, the data indicated that the planet HAT-P-33b did indeed exist.
423:, which disrupted the ability to obtain accurate measurements. As such, a greater number of radial velocity observations were collected to make the confirmation, although it was later determined that HAT-P-33b could not be determined using the
544:
alternatives that could explain the planet-like signal seen in HAT-P-33's light curve and radial velocity. The use of
Blendanal ruled out the possibilities that the signal was caused by that of a
643:
that is measured at = 0.05. This means that HAT-P-33 has 12% more iron than the amount measured in the Sun. HAT-P-33 is younger than the Sun, at an estimated age of 2.4 billion years. The
529:
observations of HAT-P-33 were conducted using the Fred
Lawrence Whipple Observatory's 1.2-meter telescope, which hosted the KeplerCam CCD instrument. This data was used to create the
1253:
681:
than HAT-P-33b exist in the system. However, at the time of HAT-P-33b's discovery, not enough radial velocity measurements had been collected to determine if this is so.
969:
830:
Hartman; Bakos; Torres; Latham; Kovács; Béky; Quinn; Mazeh; Shporer (2011). "HAT-P-32b and HAT-P-33b: Two Highly
Inflated Hot Jupiters Transiting High-Jitter Stars".
1842:
580:, contributed to the question of what factors, besides temperature, contribute to the large radii of these inflated planets. The discrepancy lies in planet
451:, or crossing in front of, their host stars. The presence of a planet in HAT-P-33's orbit had been suspected as early as 2004, although high levels of
1979:
705:, which is about 5% of the average distance between the Sun and Earth. This orbit is completed every 3.474474 days (83.39 hours). HAT-P-33b has an
697:. In other words, it is about three-fourths as massive as Jupiter, but is slightly less than twice Jupiter's size. HAT-P-33b orbits its star at an
1139:
1959:
1402:
1170:
720:
of 86.7º as seen from Earth. The planet is, thus, almost edge-on when seen from Earth. The planet has been observed to transit its host star.
455:
were detected. This jitter, or a random and shaky appearance that clouds the accuracy of measurements, made it difficult to easily verify the
1398:
515:
525:
It became apparent to the investigating science team that radial velocity data alone could not prove the existence of HAT-P-33b. As such,
647:
of the star is determined to be 4.09. All the values above are determined with the assumption that planet HAT-P-33b has an irregular, or
487:
54:
1032:
Adams, E. R.; et al. (2013). "Adaptive Optics Images. II. 12 Kepler
Objects of Interest and 15 Confirmed Transiting Planets".
1005:
32:
1954:
74:
1000:
774:
Hartman, J. D.; et al. (2011). "HAT-P-32b and HAT-P-33b: Two Highly
Inflated Hot Jupiters Transiting High-jitter Stars".
1969:
95:
503:
1085:
1930:
1925:
1920:
902:"Transiting Exoplanet Monitoring Project (TEMP). II. Refined System Parameters and Transit Timing Analysis of HAT-P-33b"
635:; the star is, in other words, 40% more massive than and 77% larger than the Sun. With an effective temperature of 6401
593:. The paper was submitted on June 6, 2011. The authors of the discovery paper of the planets suggested the usage of the
1132:
507:
511:
ability of scientists to verify this planet. After the observations, follow-ups were postponed for several years.
533:
of HAT-P-33. In doing so, a slight dimming was observed where HAT-P-33b was believed to have transited its star.
45:
370:
709:
of 1838 K, which is almost fifteen times hotter than the measured equilibrium temperature of
Jupiter (124 K).
1822:
1229:
1199:
706:
594:
536:
Using a program called
Blendanal, similar to the Blender technique used to verify the planets discovered by
270:
1974:
1156:
1125:
616:
526:
424:
1964:
589:
584:, which is far hotter than the newly discovered HAT planets and WASP-17b, but has a far smaller radius.
519:
495:
467:
215:
58:
1680:
1766:
1090:
1051:
923:
849:
793:
648:
115:
1235:
459:
of the planetary candidate's host star, which usually leads summarily to the planet's confirmation.
1847:
1831:
1346:
1166:
717:
537:
483:
167:
1741:
556:
1910:
1675:
1358:
1334:
1271:
1067:
1041:
941:
913:
865:
839:
809:
783:
655:
416:, raised the question of what (other than temperature) causes these planets to become so large.
1883:
1370:
1259:
1245:
1203:
1179:
702:
108:
959:
1869:
1772:
1731:
1059:
931:
857:
801:
346:
87:
1726:
1736:
1716:
671:
667:
644:
499:
471:
456:
354:
1055:
927:
853:
797:
1875:
1010:
698:
694:
678:
541:
448:
444:
432:
286:
135:
80:
514:
Between
September 2008 and December 2010, twenty-two spectra were collected using the
1948:
1746:
1721:
1711:
1438:
1411:
1071:
945:
869:
861:
813:
805:
545:
1063:
690:
636:
632:
313:
1099:
443:
HAT-P-33b's existence was first suggested after observations by the six-telescope
1777:
1514:
1433:
1223:
1212:
640:
598:
549:
530:
428:
377:
936:
901:
1663:
1658:
1648:
1643:
1636:
1631:
1626:
1621:
1616:
1590:
1585:
1578:
1573:
1568:
1563:
1558:
1553:
1541:
1536:
1473:
1427:
628:
624:
491:
1864:
1810:
1805:
1800:
1795:
1750:
1670:
1653:
1611:
1595:
1548:
1531:
1526:
1521:
1503:
1498:
1493:
1488:
1443:
1307:
1193:
659:
573:
413:
236:
1695:
1690:
1685:
1483:
1478:
1468:
1463:
1382:
1295:
1283:
610:
587:
The discoveries of HAT-P-33b and HAT-P-32b were reported together in the
581:
577:
565:
479:
409:
405:
256:
1889:
1458:
1453:
1328:
1323:
1318:
561:
494:
exhibiting a slight rotation. Several of its parameters, including its
327:
639:, HAT-P-33 is hotter than the Sun. It is also more metal-rich, with a
964:
620:
452:
420:
419:
HAT-P-33b was difficult to confirm because its star experiences high
50:
462:
918:
601:
of HAT-P-33b behind its star to better define its characteristics.
1761:
1187:
1046:
844:
788:
555:
461:
187:
1787:
1117:
1095:
490:
in
Arizona. The collected data found that the star was a single
343:
298:
1121:
160:
447:
collaboration, a project that searches the sky for planets
427:. The planet's confirmation came about after the planet's
572:
The discoveries of the high-radii planets HAT-P-33b and
431:
was collected, and the
Blendanal process ruled out most
540:, the astronomers observing HAT-P-33 hoped to rule out
1856:
1819:
1786:
1704:
1397:
1243:
1165:
376:
352:
324:
297:
268:
263:
252:
234:
213:
185:
166:
133:
114:
93:
86:
72:
64:
44:
31:
26:
658:of 11.89. It cannot be seen from Earth with the
677:It is possible that other planets with shorter
769:
767:
765:
763:
761:
759:
757:
755:
753:
1133:
970:Centre de données astronomiques de Strasbourg
751:
749:
747:
745:
743:
741:
739:
737:
735:
733:
8:
21:
1140:
1126:
1118:
895:
893:
891:
889:
887:
885:
883:
881:
879:
1045:
935:
917:
843:
787:
548:or a mixture between a bright star and a
825:
823:
729:
470:was used to collect data on HAT-P-33's
627:) away from Earth. The star has 1.403
506:at a 1.93-meter telescope at France's
20:
1880:(end of mission; Mar 2010 / May 2011)
994:
992:
990:
988:
986:
689:HAT-P-33b is a planet that has 0.764
7:
900:Wang, Yong-Hao; et al. (2017).
516:High Resolution Echelle Spectrometer
615:HAT-P-33, or GSC 2461-00988, is an
560:HAT-P-33b is 1.8 times the size of
482:of HAT-P-33 was composed using the
14:
619:star that lies approximately 401
564:(left), and slightly larger than
488:Fred Lawrence Whipple Observatory
1916:
1915:
1904:
1821:
1401:
1234:
1228:
1222:
1169:
1006:Extrasolar Planets Encyclopaedia
502:, were found. Additionally, the
1980:Exoplanets discovered by HATNet
1190:(mission to the Moon; Sep 2011)
518:(HIRES) instrument at Hawaii's
1:
1960:Exoplanets discovered in 2011
1931:Category:2012 in outer space
1926:Category:2011 in outer space
1921:Category:2010 in outer space
1892:orbital insertion; Jul 2011)
1872:orbital insertion; Apr 2011)
404:is a planet in the orbit of
1843:45P/Honda–Mrkos–Pajdušáková
1215:(mission to Mars; Nov 2011)
1209:(mission to Mars; Nov 2011)
1184:(Jupiter orbiter; Aug 2011)
504:SOPHIE échelle spectrograph
216:Argument of periastron
1996:
862:10.1088/0004-637X/742/1/59
806:10.1088/0004-637X/742/1/59
608:
508:Haute-Provence Observatory
1899:
1254:Asteroid close approaches
1220:
1196:(Mars orbiter); Nov 2011)
1153:
1064:10.1088/0004-6256/146/1/9
1001:"Notes for star HAT-P-33"
832:The Astrophysical Journal
776:The Astrophysical Journal
395:
136:Orbital period (sidereal)
1034:The Astronomical Journal
937:10.3847/1538-3881/aa7519
906:The Astronomical Journal
546:hierarchical triple star
264:Physical characteristics
1200:Mars Science Laboratory
999:Jean Schneider (2011).
707:equilibrium temperature
595:Spitzer Space Telescope
188:Time of periastron
88:Orbital characteristics
1955:Gemini (constellation)
1911:Outer space portal
1098:. 2011. Archived from
662:because it is so dim.
569:
475:
425:radial velocity method
68:Published June 6, 2011
1970:Transiting exoplanets
590:Astrophysical Journal
576:, along with that of
559:
520:W.M. Keck Observatory
496:effective temperature
468:W.M. Keck Observatory
465:
1167:Space probe launches
1091:Ames Research Center
1086:"Kepler Discoveries"
1848:C/2011 W3 (Lovejoy)
1767:SDSS J102915+172927
1056:2013AJ....146....9A
928:2017AJ....154...49W
854:2011ApJ...742...59H
798:2011ApJ...742...59H
718:orbital inclination
484:digital speedometer
65:Discovery date
46:Discovery site
23:
1676:MOA-2009-BLG-387Lb
656:apparent magnitude
570:
476:
33:Discovered by
1939:
1938:
1857:Space exploration
716:HAT-P-33b has an
486:at the 1.5-meter
399:
398:
259:(GSC 02461-00988)
16:Extrasolar planet
1987:
1919:
1918:
1909:
1908:
1907:
1837:
1825:
1773:moons of Jupiter
1758:
1756:
1755:
1681:PSR J1719−1438 b
1432:habitability of
1405:
1390:
1388:
1387:
1378:
1376:
1375:
1371:(549948) 2011 WL
1366:
1364:
1363:
1359:(308635) 2005 YU
1354:
1352:
1351:
1347:(436724) 2011 UW
1342:
1340:
1339:
1335:(415029) 2011 UL
1315:
1313:
1312:
1303:
1301:
1300:
1291:
1289:
1288:
1279:
1277:
1276:
1272:(471240) 2011 BT
1267:
1265:
1264:
1260:(367789) 2011 AG
1238:
1232:
1226:
1173:
1142:
1135:
1128:
1119:
1112:
1111:
1109:
1107:
1082:
1076:
1075:
1049:
1029:
1023:
1022:
1020:
1018:
1013:on July 22, 2011
1009:. Archived from
996:
981:
980:
978:
976:
956:
950:
949:
939:
921:
897:
874:
873:
847:
827:
818:
817:
791:
771:
699:average distance
654:HAT-P-33 has an
478:As a start, the
391:
390:
389:
369:
368:
367:
342:
341:
340:
312:
311:
310:
285:
284:
283:
248:
246:
239:
230:
229:
228:
209:
208:
207:
200:
197:
181:
180:
179:
159:
158:
155:
151:
148:
145:
129:
128:
127:
107:
105:
75:Detection method
24:
1995:
1994:
1990:
1989:
1988:
1986:
1985:
1984:
1945:
1944:
1942:
1940:
1935:
1905:
1903:
1895:
1852:
1836:
1832:
1815:
1782:
1753:
1752:
1749:
1737:Kerberos (moon)
1732:ULAS J1120+0641
1700:
1393:
1385:
1384:
1381:
1373:
1372:
1369:
1361:
1360:
1357:
1349:
1348:
1345:
1337:
1336:
1333:
1310:
1309:
1306:
1298:
1297:
1294:
1286:
1285:
1282:
1274:
1273:
1270:
1262:
1261:
1258:
1239:
1233:
1227:
1218:
1161:
1160:
1149:
1146:
1116:
1115:
1105:
1103:
1084:
1083:
1079:
1031:
1030:
1026:
1016:
1014:
998:
997:
984:
974:
972:
958:
957:
953:
899:
898:
877:
829:
828:
821:
773:
772:
731:
726:
687:
685:Characteristics
679:orbital periods
672:MMT Observatory
668:adaptive optics
645:surface gravity
613:
607:
597:to observe the
500:surface gravity
472:radial velocity
457:radial velocity
441:
387:
385:
384:
382:
365:
363:
362:
360:
357:
355:Surface gravity
338:
336:
335:
333:
330:
319:
316:
308:
306:
305:
303:
292:
289:
281:
279:
278:
276:
273:
244:
242:
235:
226:
224:
223:
221:
218:
205:
203:
202:
198:
195:
193:
190:
177:
175:
174:
172:
156:
153:
149:
146:
143:
141:
138:
125:
123:
122:
120:
103:
101:
98:
96:Semi-major axis
77:
17:
12:
11:
5:
1993:
1991:
1983:
1982:
1977:
1972:
1967:
1962:
1957:
1947:
1946:
1937:
1936:
1934:
1933:
1913:
1900:
1897:
1896:
1894:
1893:
1881:
1873:
1860:
1858:
1854:
1853:
1851:
1850:
1845:
1840:
1834:
1828:
1826:
1817:
1816:
1814:
1813:
1808:
1803:
1798:
1792:
1790:
1784:
1783:
1781:
1780:
1775:
1769:
1764:
1759:
1744:
1742:PSR J1719−1438
1739:
1734:
1729:
1724:
1719:
1717:Swift J1644+57
1714:
1708:
1706:
1702:
1701:
1699:
1698:
1693:
1688:
1683:
1678:
1673:
1668:
1667:
1666:
1661:
1651:
1646:
1641:
1640:
1639:
1634:
1629:
1624:
1619:
1609:
1608:
1607:
1604:
1601:
1593:
1588:
1583:
1582:
1581:
1576:
1571:
1566:
1561:
1556:
1546:
1545:
1544:
1539:
1529:
1524:
1519:
1518:
1517:
1512:
1509:
1501:
1496:
1491:
1486:
1481:
1476:
1471:
1466:
1461:
1456:
1451:
1446:
1441:
1436:
1430:
1425:
1424:
1423:
1420:
1417:
1408:
1406:
1395:
1394:
1392:
1391:
1379:
1367:
1355:
1343:
1331:
1326:
1321:
1316:
1304:
1292:
1280:
1268:
1256:
1250:
1248:
1241:
1240:
1221:
1219:
1217:
1216:
1210:
1197:
1191:
1185:
1176:
1174:
1163:
1162:
1155:
1154:
1151:
1150:
1147:
1145:
1144:
1137:
1130:
1122:
1114:
1113:
1077:
1024:
982:
951:
875:
819:
728:
727:
725:
722:
691:Jupiter masses
686:
683:
674:was negative.
609:Main article:
606:
603:
542:false positive
440:
437:
433:false positive
397:
396:
393:
392:
380:
374:
373:
358:
353:
350:
349:
331:
325:
322:
321:
317:
314:
301:
295:
294:
290:
287:
274:
269:
266:
265:
261:
260:
254:
250:
249:
240:
237:Semi-amplitude
232:
231:
219:
214:
211:
210:
191:
186:
183:
182:
170:
164:
163:
139:
134:
131:
130:
118:
112:
111:
99:
94:
91:
90:
84:
83:
81:transit method
78:
73:
70:
69:
66:
62:
61:
48:
42:
41:
35:
29:
28:
15:
13:
10:
9:
6:
4:
3:
2:
1992:
1981:
1978:
1976:
1975:Giant planets
1973:
1971:
1968:
1966:
1963:
1961:
1958:
1956:
1953:
1952:
1950:
1943:
1932:
1928:
1927:
1922:
1914:
1912:
1902:
1901:
1898:
1891:
1887:
1886:
1882:
1879:
1878:
1874:
1871:
1867:
1866:
1862:
1861:
1859:
1855:
1849:
1846:
1844:
1841:
1839:
1830:
1829:
1827:
1824:
1818:
1812:
1809:
1807:
1804:
1802:
1799:
1797:
1794:
1793:
1791:
1789:
1785:
1779:
1776:
1774:
1770:
1768:
1765:
1763:
1760:
1757:
1748:
1747:Uranus trojan
1745:
1743:
1740:
1738:
1735:
1733:
1730:
1728:
1725:
1723:
1722:Kronberger 61
1720:
1718:
1715:
1713:
1712:UDFj-39546284
1710:
1709:
1707:
1703:
1697:
1694:
1692:
1689:
1687:
1684:
1682:
1679:
1677:
1674:
1672:
1669:
1665:
1662:
1660:
1657:
1656:
1655:
1652:
1650:
1647:
1645:
1642:
1638:
1635:
1633:
1630:
1628:
1625:
1623:
1620:
1618:
1615:
1614:
1613:
1610:
1605:
1602:
1599:
1598:
1597:
1594:
1592:
1589:
1587:
1584:
1580:
1577:
1575:
1572:
1570:
1567:
1565:
1562:
1560:
1557:
1555:
1552:
1551:
1550:
1547:
1543:
1540:
1538:
1535:
1534:
1533:
1530:
1528:
1525:
1523:
1520:
1516:
1513:
1510:
1507:
1506:
1505:
1502:
1500:
1497:
1495:
1492:
1490:
1487:
1485:
1482:
1480:
1477:
1475:
1472:
1470:
1467:
1465:
1462:
1460:
1457:
1455:
1452:
1450:
1447:
1445:
1442:
1440:
1439:Gliese 3634 b
1437:
1435:
1431:
1429:
1426:
1421:
1418:
1415:
1414:
1413:
1412:82 G. Eridani
1410:
1409:
1407:
1404:
1400:
1396:
1389:
1380:
1377:
1368:
1365:
1356:
1353:
1344:
1341:
1332:
1330:
1327:
1325:
1322:
1320:
1317:
1314:
1305:
1302:
1293:
1290:
1281:
1278:
1269:
1266:
1257:
1255:
1252:
1251:
1249:
1247:
1242:
1237:
1231:
1225:
1214:
1211:
1208:
1206:
1201:
1198:
1195:
1192:
1189:
1186:
1183:
1182:
1178:
1177:
1175:
1172:
1168:
1164:
1158:
1152:
1148:2011 in space
1143:
1138:
1136:
1131:
1129:
1124:
1123:
1120:
1102:on 2010-05-27
1101:
1097:
1093:
1092:
1087:
1081:
1078:
1073:
1069:
1065:
1061:
1057:
1053:
1048:
1043:
1039:
1035:
1028:
1025:
1012:
1008:
1007:
1002:
995:
993:
991:
989:
987:
983:
971:
967:
966:
961:
955:
952:
947:
943:
938:
933:
929:
925:
920:
915:
911:
907:
903:
896:
894:
892:
890:
888:
886:
884:
882:
880:
876:
871:
867:
863:
859:
855:
851:
846:
841:
837:
833:
826:
824:
820:
815:
811:
807:
803:
799:
795:
790:
785:
781:
777:
770:
768:
766:
764:
762:
760:
758:
756:
754:
752:
750:
748:
746:
744:
742:
740:
738:
736:
734:
730:
723:
721:
719:
714:
710:
708:
704:
700:
696:
695:Jupiter radii
692:
684:
682:
680:
675:
673:
669:
663:
661:
657:
652:
650:
646:
642:
638:
634:
630:
626:
622:
618:
612:
604:
602:
600:
596:
592:
591:
585:
583:
579:
575:
567:
563:
558:
554:
551:
547:
543:
539:
534:
532:
528:
523:
521:
517:
512:
509:
505:
501:
497:
493:
489:
485:
481:
473:
469:
464:
460:
458:
454:
450:
449:in transit of
446:
438:
436:
434:
430:
426:
422:
417:
415:
411:
407:
403:
394:
381:
379:
375:
372:
359:
356:
351:
348:
345:
332:
329:
323:
320:
302:
300:
296:
293:
275:
272:
267:
262:
258:
255:
251:
241:
238:
233:
220:
217:
212:
192:
189:
184:
171:
169:
165:
162:
140:
137:
132:
119:
117:
113:
110:
100:
97:
92:
89:
85:
82:
79:
76:
71:
67:
63:
60:
56:
52:
49:
47:
43:
40:
36:
34:
30:
25:
19:
1965:Hot Jupiters
1941:
1924:
1884:
1876:
1863:
1448:
1428:Gliese 433 b
1204:
1180:
1104:. Retrieved
1100:the original
1089:
1080:
1037:
1033:
1027:
1015:. Retrieved
1011:the original
1004:
973:. Retrieved
963:
954:
909:
905:
835:
831:
779:
775:
715:
711:
688:
676:
664:
653:
629:solar masses
614:
588:
586:
571:
535:
524:
513:
477:
442:
418:
401:
400:
116:Eccentricity
38:
18:
1778:GRB 111209A
1727:WD 0806−661
1705:Discoveries
1499:HD 137388 b
1494:HD 131496 b
1489:HD 100655 b
1434:Gliese 581d
1213:Fobos-Grunt
641:metallicity
633:solar radii
625:light years
599:occultation
550:binary star
531:light curve
527:photometric
435:scenarios.
429:light curve
378:Temperature
271:Mean radius
168:Inclination
1949:Categories
1649:Kepler-39b
1644:Kepler-22b
1591:Kepler-16b
1586:Kepler-14b
1484:HD 98219 b
1479:HD 96063 b
1474:HD 85512 b
1469:HD 82886 b
1464:HD 30856 b
1399:Exoplanets
960:"HAT-P-33"
919:1705.08605
724:References
701:of 0.0503
693:and 1.827
631:and 1.777
492:dwarf star
1865:MESSENGER
1833:P/2011 NO
1811:SN 2011fe
1806:SN 2011dh
1801:SN 2011by
1796:SN 2010lt
1671:LkCa 15 b
1654:Kepler-70
1612:Kepler-20
1596:Kepler-18
1549:Kepler-11
1532:Kepler-10
1527:Kepler-9d
1522:HR 7722 c
1504:HIP 57274
1459:HD 7199 b
1454:HD 1502 b
1449:HAT-P-33b
1444:HAT-P-32b
1244:Selected
1205:Curiosity
1194:Yinghuo-1
1072:119117620
1047:1305.6548
946:119245125
912:(2). 49.
870:118590713
845:1106.1212
838:(1): 59.
814:118590713
789:1106.1212
782:(1). 59.
660:naked eye
651:, orbit.
649:eccentric
605:Host star
574:HAT-P-32b
439:Discovery
414:HAT-P-32b
402:HAT-P-33b
27:Discovery
22:HAT-P-33b
1838:(Elenin)
1696:WASP-44b
1691:WASP-43b
1686:WASP-39b
1159: »
1040:(1). 9.
975:14 April
611:HAT-P-33
582:WASP-18b
578:WASP-17b
568:(right).
566:WASP-17b
480:spectrum
410:WASP-17b
406:HAT-P-33
257:HAT-P-33
37:Hartman
1870:Mercury
1820:Comets
1751:2011 QF
1383:2011 XC
1329:2011 MD
1324:2009 BD
1319:2011 GA
1308:2011 EO
1296:2011 ES
1284:2011 CQ
1106:15 June
1052:Bibcode
1017:15 June
924:Bibcode
850:Bibcode
794:Bibcode
670:at the
623:(1,310
621:parsecs
562:Jupiter
328:density
1877:Spirit
1070:
965:SIMBAD
944:
868:
812:
617:F-type
538:Kepler
453:jitter
445:HATnet
421:jitter
339:−0.042
337:+0.053
126:−0.096
106:0.0018
102:0.0505
51:HATNet
39:et al.
1890:Vesta
1788:Novae
1762:U1.11
1207:rover
1188:GRAIL
1068:S2CID
1042:arXiv
942:S2CID
914:arXiv
866:S2CID
840:arXiv
810:S2CID
784:arXiv
366:−0.11
364:+0.10
334:0.134
326:Mean
309:−0.12
307:+0.13
282:−0.20
280:+0.26
206:−0.23
204:+0.22
152:0.000
142:3.474
124:+0.11
121:0.180
1885:Dawn
1246:NEOs
1181:Juno
1157:2012
1108:2011
1096:NASA
1019:2011
977:2018
498:and
466:The
412:and
388:−120
386:+140
383:1920
371:m/s²
361:2.70
304:0.72
299:Mass
277:1.87
253:Star
178:−1.3
176:+1.2
173:88.2
59:Keck
55:FLWO
1350:158
1060:doi
1038:146
932:doi
910:154
858:doi
836:742
802:doi
780:742
227:−34
225:+33
201:.20
199:046
196:457
154:000
144:474
1951::
1929:—
1923:—
1771:2
1754:99
1362:55
1338:21
1311:40
1275:15
1202:/
1094:.
1088:.
1066:.
1058:.
1050:.
1036:.
1003:.
985:^
968:.
962:.
940:.
930:.
922:.
908:.
904:.
878:^
864:.
856:.
848:.
834:.
822:^
808:.
800:.
792:.
778:.
732:^
703:AU
347:cm
247:12
243:78
222:88
157:88
147:72
109:AU
57:)/
1888:(
1868:(
1835:1
1664:c
1659:b
1637:f
1632:e
1627:d
1622:c
1617:b
1606:d
1603:c
1600:b
1579:g
1574:f
1569:e
1564:d
1559:c
1554:b
1542:c
1537:b
1515:d
1511:c
1508:b
1422:d
1419:c
1416:b
1386:2
1374:2
1299:4
1287:1
1263:5
1141:e
1134:t
1127:v
1110:.
1074:.
1062::
1054::
1044::
1021:.
979:.
948:.
934::
926::
916::
872:.
860::
852::
842::
816:.
804::
796::
786::
637:K
474:.
344:g
318:J
315:M
291:J
288:R
245:±
194:2
161:d
150:±
104:±
53:(
Text is available under the Creative Commons Attribution-ShareAlike License. Additional terms may apply.