ライフサイエンスコーパス: orbital period

1 een eccentricity, host star metallicity, and orbital period.

2 lated, Earth-sized planet with a roughly 1-d orbital period.

3 ng a direct measure of the planet's size and orbital period.

4 5-hour pulse of 0.1% amplitude occurs every orbital period.

5 art that is also apparently modulated on the orbital period.

6 period is changing and is different from its orbital period.

7 y in a regular fashion on a timescale of one orbital period.

8 mined identical values for the change in the orbital period.

9 netary systems, mostly about their sizes and orbital periods.

10 ing the distribution of exoplanet masses and orbital periods.

11 form a near-resonant chain, such that their orbital periods (1.51, 2.42, 4.04, 6.06, 9.1 and 12.35 d

12 with moderate-mass companions and very short orbital periods(9), but, hitherto, no such system was kn

13 s of these properties and the planet's short orbital period and high equilibrium temperature, we show

14 n belt, where it spends more than 1/3 of its orbital period and it may undergo many more collisions t

15 to 1 of 14 Be X-ray binaries that have known orbital periods and eccentricities(7).

16 ucing systems with short spin periods, short orbital periods and low eccentricities.

17 with different characteristic spin periods, orbital periods and orbital eccentricities.

18 d to the planet's as well as to the binary's orbital periods are present in a variety of climate indi

19 aused a variation of about 33 minutes in its orbital period around Didymos and demonstrated the feasi

20 sigma) kilometers and a 15.774 +/- 0.002 day orbital period around Eris.

21 Until now, the absence of planets with short orbital periods around post-expansion, core-helium-burni

22 stron distance that it may circularize at an orbital period as short as a few days through tidal diss

23 s in longitude that are forced at the 88-day orbital period, as predicted by theory.

24 Stars with short orbital periods at the center of our Galaxy offer a powe

25 Five candidates have orbital periods below 1.0 day, constituting a new class

26 from a hydrogen-rich star, only a dozen have orbital periods below 75 minutes(1-9).

27 We discovered 16 candidates with orbital periods between 0.4 and 4.2 days, five of which

28 hat reveal six transiting planets, five with orbital periods between 10 and 47 days and a sixth plane

29 General relativity(1) predicts that short-orbital-period binaries emit considerable amounts of gra

30 wide hierarchical triple hosting a 62-minute orbital period black widow candidate, the optical flux o

31 In this case, however, the long orbital period (compared with other white dwarfs with cl

32 ral mechanisms, contributing to the observed orbital-period distribution, where many planets are not

33 n the original 'black widow', the eight-hour orbital period eclipsing pulsar PSR J1959+2048(1), high-

34 sured from the decrease in starlight and its orbital period from the time between transits.

35 sizes between 0.37 and 1.6 Jupiter radii and orbital periods from 3.2 to 4.9 days were discovered.

36 se eclipsing planetary systems, over half an orbital period, from which we can construct a 'map' of t

37 observations of ZTF J1813+4251, a 51-minute-orbital-period, fully eclipsing binary system consisting

38 vitating protoplanets arise after a few disk orbital periods if cooling is efficient enough to mainta

39 This orbital period implies that the mass-donor star must be

40 y period of the giant is consistent with the orbital period, indicating star spots and tidal synchron

41 The exoplanet's orbital period is 3.7 days, and its minimum mass is 13.2

42 The outer planet's orbital period is 303.2 days, and although the planet is

43 Instead, we propose that a long orbital period is a key condition for these large-amplit

44 the F ring, it draws out ring material; one orbital period later, this affected region has undergone

45 he occurrence rate of close-in planets (with orbital periods less than 50 days), based on precise Dop

46 he domain from 5 to 30 Earth masses and with orbital periods less than 50 days.

47 es tightly packed systems with planets whose orbital periods may be expressed as ratios of small inte

48 net candidates (Jupiter-size candidates with orbital periods near 3 d) identified in the Kepler data

49 ort the discovery of planet WASP-18b with an orbital period of 0.94 days and a mass of ten Jupiter ma

50 We detect a transiting rocky planet with an orbital period of 1.467 days around the nearby red dwarf

51 The orbital period of 1.755 +/- 0.007 days and semimajor axi

52 ary SDSS J065133.338+284423.37, which has an orbital period of 12.75 minutes.

53 The planet has an orbital period of 3.35 days and a minimum mass of 1.14 t

54 known planets, the innermost of which has an orbital period of 4.617 days and a mass at least 0.69 th

55 With an orbital period of 49.5 days, 18 transits of the inner pl

56 SR J1953+1844 (M71E) that show it to have an orbital period of 53.3 minutes and a companion with a ma

57 ary system, ZTF J153932.16+502738.8, with an orbital period of 6.91 minutes.

58 The long orbital period of 78.9 days shows that this is a wide bi

59 The transiting planet, AU Mic b, has an orbital period of 8.46 days, an orbital distance of 0.07

60 o known as KELT-9), which reveal a close-in (orbital period of about 1.48 days) transiting giant plan

61 HD 66051 is an eclipsing system with an orbital period of about 4.75 d that exhibits out-of-ecli

62 ts Dinkinesh at a distance of 3.1 km with an orbital period of about 52.7 h and is tidally locked.

63 eparated by approximately 0.1 parsec with an orbital period of approximately 100 years.

64 A change in orbital period of approximately 7 min was expected if th

65 after the infrared brightening, implying an orbital period of at least that duration.

66 Here we report the change in the orbital period of Dimorphos as a result of the DART kine

67 addition to having successfully changed the orbital period of Dimorphos(3), demonstrated the activat

68 y asteroid (65803) Didymos, and changing the orbital period of Dimorphos.

69 dels(5), falling below the 80-minute minimum orbital period of hydrogen-rich systems.

70 The co-existence at the same orbital period of novalike binaries and dwarf novae-whic

71 In addition, the orbital period of one of the observed stars could be as

72 The median semi-major axis and orbital period of planets in phase space overdensities a

73 If the orbital period of the binary is short enough, energy los

74 If the orbital period of the black-hole binary matches this val

75 62.0 +/- 2.5 days, which we interpret as the orbital period of the ULX binary.

76 of an outer (non-transiting) planet with an orbital period of ~ 10 d.

77 The system has an orbital period of ~83 days and near-zero eccentricity.

78 -like stars harbor an Earth-size planet with orbital periods of 200-400 d.

79 The radii and orbital periods of 4,000+ confirmed/candidate exoplanets

80 The two planets have orbital periods of 9.3 and 21.8 days.

81 city distribution, with all but three having orbital periods of approximately 1,000 days.

82 ts in the same orbital plane as Charon, with orbital periods of approximately 38 days (P1) and approx

83 companion masses of about 0.1-0.4 M((.)) and orbital periods of less than 1 day(8).

84 The orbital periods of the two new moons are nearly integer

85 ion light curve is modulated over the binary orbital period owing to relativistic beaming.

86 (passing perihelion in 1989 in its 248-year orbital period), owing to the extreme sensitivity of the

87 = 0.2318 +/- 0.0013 R(middle dot in circle); orbital period P(1) = 1.76713 +/- 0.00019 days] on an ec

88 rth-size planets is constant with increasing orbital period (P), within equal intervals of logP up to

89 warfs are often found in binary systems with orbital periods ranging from tens of minutes to hours in

90 nominal cases, pre-impact predictions of the orbital period reduction ranged from roughly 8.8 to 17 m

91 Those in resonance (with their orbital periods related by a ratio of small integers) ar

92 periods tidally spin-synchronized with their orbital periods, resulting in permanent star-facing hemi

93 Planets with short orbital periods (roughly under 10 days) are common aroun

94 nown transitional CV is expected to reach an orbital period short enough to account for most of the h

95 Ultrashort-period (USP) exoplanets have orbital periods shorter than 1 day.

96 e of planet formation generates planets with orbital periods shorter than 100 days and masses substan

97 anet occurrence rates as a function of size, orbital period, star type, and insolation flux.

98 latively high mass of the donor star for its orbital period suggests that current evolutionary models

99 s of the two stars are tidally locked to the orbital period, the rapid rotation drives a magnetic dyn

100 sence of a basin, because, averaged over its orbital period, those are Pluto's coldest regions.

101 ed to become a helium CV binary, reaching an orbital period under 20 minutes, rendering ZTF J1813+425

102 mall, 1-2 R plus sign in circle planets with orbital periods under 100 d, and 11% have 1-2 R plus sig

103 part of the large disk in binaries with long orbital periods will have surface densities too low to m