ライフサイエンスコーパス: orbital period

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

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

3 5-hour pulse of 0.1% amplitude occurs every orbital period.

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

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

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

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

8 ing the distribution of exoplanet masses and orbital periods.

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

44 62.0 +/- 2.5 days, which we interpret as the orbital period of the ULX binary.

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

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

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

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

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

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

51 = 0.2318 +/- 0.0013 R(middle dot in circle); orbital period P(1) = 1.76713 +/- 0.00019 days] on an ec

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

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

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

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

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

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

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

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

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

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