Orbit, A Planetary Orbit Code

AbstractWe show that a consistent fit to observed secondary eclipse data for several strongly irradiated transiting planets demands a temperature inversion (stratosphere) at altitude. Such a thermal inversion significantly influences the planet/star contrast ratios at the secondary eclipse, their wavelength dependences, and, importantly, the day-night flux contrast during a planetary orbit. The presence of the thermal inversion/stratosphere seems to roughly correlate with the stellar flux at the planet. Such temperature inversions might be caused by an upper-atmosphere absorber whose exact nature is still uncertain.

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“Planetary Orbit” Systems Composed of Cycloparaphenylenes

The Journal of Organic Chemistry ◽

10.1021/acs.joc.6b00339 ◽

2016 ◽

Vol 81 (11) ◽

pp. 4559-4565 ◽

Cited By ~ 11

Author(s):

Steven M. Bachrach ◽

Zeina-Christina Zayat

Keyword(s):

Planetary Orbit

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STELLAR ROTATION-PLANETARY ORBIT PERIOD COMMENSURABILITY IN THE HAT-P-11 SYSTEM

The Astrophysical Journal ◽

10.1088/0004-637x/788/1/1 ◽

2014 ◽

Vol 788 (1) ◽

pp. 1 ◽

Cited By ~ 26

Author(s):

Bence Béky ◽

Matthew J. Holman ◽

David M. Kipping ◽

Robert W. Noyes

Keyword(s):

Planetary Orbit ◽

Stellar Rotation ◽

Orbit Period

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XIX.—Elliptic Expansions

Proceedings of the Royal Society of Edinburgh ◽

10.1017/s037016460002397x ◽

1923 ◽

Vol 42 ◽

pp. 318-318

Author(s):

R. T. A. Innes

Keyword(s):

Radius Vector ◽

Planetary Orbit ◽

True Anomaly ◽

The Mean ◽

Image Position ◽

First Time

AbstractIn seeking the expansion of the equation of the centre, and the logarithm of the radius vector in a planetary orbit, in terms of the mean anomaly, the following expressions are obtained:—where g is the mean anomaly, andMr Innes remarks: “It is shown for the first time, I believe, that the expansion for the true anomaly in terms of the mean (equation of the centre) can be derived quite easily from the addition of the two simple expansionsand the two series have most simple recurrence expressions.”The MS. containing the proofs of these expressions, with further developments, is in the hands of the Society.

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First observation of planet-induced X-ray emission: The system HD 179949

Proceedings of the International Astronomical Union ◽

10.1017/s1743921308016414 ◽

2007 ◽

Vol 3 (S249) ◽

pp. 79-81 ◽

Cited By ~ 6

Author(s):

S. H. Saar ◽

M. Cuntz ◽

V. L. Kashyap ◽

J. C. Hall

Keyword(s):

Giant Planet ◽

Planetary Orbit ◽

X Ray ◽

Background Star

AbstractWe present the first observation of planet-induced stellar X-ray activity, identified for the HD 179949 system, using Chandra / ACIS-S. The HD 179949 system consists of a close-in giant planet orbiting an F9 V star. Previous ground-based observations already showed enhancements in Ca II K in phase with the planetary orbit. We find an ∼30% increase in the X-ray flux over quiescent levels coincident with the phase of the Ca II enhancements. There is also a trend for the emission to be hotter at increased fluxes, confirmed by modeling, showing the enhancement at ∼1 keV compared to ∼0.4 keV for the background star.

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Detection of Exomoons Inside the Habitable Zone

Proceedings of the International Astronomical Union ◽

10.1017/s1743921313012751 ◽

2012 ◽

Vol 8 (S293) ◽

pp. 168-170

Author(s):

Luis Ricardo M. Tusnski ◽

Adriana Valio

Keyword(s):

The Other ◽

Planetary Orbit ◽

Habitable Zone ◽

The Moon ◽

Stellar Activity ◽

Orbital Parameters ◽

Hot Jupiters ◽

Habitable Zones ◽

Observational Bias ◽

Host Stars

AbstractSince the discovery of the first exoplanets, those most adequate for life to begin and evolve have been sought. Due to observational bias, however, most of the discovered planets so far are gas giants, precluding their habitability. However, if these hot Jupiters are located in the habitable zones of their host stars, and if rocky moons orbit them, then these moons may be habitable. In this work, we present a model for planetary transit simulation considering the presence of moons around a planet. The moon orbit is considered to be circular and coplanar with the planetary orbit. The other physical and orbital parameters of the star, planet, and moon, can be adjusted in each simulation. It is possible to simulate as many successive transits as desired. Since the presence of spots on the surface of the star may produce a signal similar to that of the presence of a moon, our model also allows for the inclusion of starspots. The goal is to determine the criteria for detectability of moons using photometry with the CoRoT and Kepler telescopes taking into account the stellar activity.

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Tuning in to the radio environment of HD189733b

Proceedings of the International Astronomical Union ◽

10.1017/s1743921319009773 ◽

2019 ◽

Vol 15 (S354) ◽

pp. 305-309

Author(s):

R. D. Kavanagh ◽

A. A. Vidotto ◽

D. Ó Fionnagáin ◽

V. Bourrier ◽

R. Fares ◽

...

Keyword(s):

Magnetic Field ◽

Radio Emission ◽

Flux Density ◽

Stellar Wind ◽

Planetary Orbit ◽

Close Proximity ◽

Peak Flux ◽

Detection Capabilities ◽

Reconstructed Surface ◽

Hot Jupiter

AbstractThe hot Jupiter HD189733b is expected to be a source of strong radio emission, due to its close proximity to its magnetically active host star. Here, we model the stellar wind of its host star, based on reconstructed surface stellar magnetic field maps. We use the local stellar wind properties at the planetary orbit obtained from our models to compute the expected radio emission from the planet. Our findings show that the planet emits with a peak flux density within the detection capabilities of LOFAR. However, due to absorption by the stellar wind itself, this emission may be attenuated significantly. We show that the best time to observe the system is when the planet is near primary transit of the host star, as the attenuation from the stellar wind is lowest in this region.

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