scholarly journals On the Origin of Commensurabilities in the Solar System--II The Orbital Period Relation

1968 ◽  
Vol 141 (3) ◽  
pp. 363-376 ◽  
Author(s):  
S. F. Dermott
Keyword(s):  
Solar System ◽  
Orbital Period ◽  
Period Relation

A Recurrence Time versus Orbital Period Relation for the Z Camelopardalis Stars

2005 ◽  
Vol 117 (835) ◽  
pp. 931-937 ◽  
Author(s):  
Allen W. Shafter ◽  
John K. Cannizzo ◽  
Elizabeth O. Waagen
Keyword(s):  
Orbital Period ◽  
Recurrence Time ◽  
Period Relation

scholarly journals The Nasa Solar Probe Mission: In Situ Determination of Interplanetary Out-of-The Ecliptic and Near-Solar Dust Environments

1991 ◽  
Vol 126 ◽  
pp. 29-32
Author(s):  
Bruce T. Tsurutani ◽  
James E. Randolph
Keyword(s):  
Solar Cycle ◽  
Solar System ◽  
Solar Eclipse ◽  
Orbital Period ◽  
High Velocity ◽  
Scientific Community ◽  
The Sun ◽  
Probe Mission

AbstractThe NASA Solar Probe mission will be one of the most exciting dust missions ever flown and will lead to a revolutionary advance in our understanding of dust within our solar system. Solar Probe will map the dust environment from the orbit of Jupiter (5 AU), to within 4 solar radii of the sun’s center. The region between 0.3 AU and 4 Rshas never been visited before, so the 10 days that the spacecraft spends during each (of the two) orbit is purely exploratory in nature. Solar Probe will also reach heliographic latitudes as high as ~ 15 to 28 above (below) the ecliptic on its trajectory inbound (outbound) to (from) the sun. This, in addition to the ESA/NASA Ulysses mission, will help determine the out-of-the-ecliptic dust environment. A post-perihelion burn will reduce the satellite orbital period to 2.5 years about the sun. A possible extended mission would allow data reception for 2 more revolutions, mapping out a complete solar cycle. Because the near-solar dust environment is not well understood (or is controversial at best), and it is very important to have better knowledge of the dust environment to protect Solar Probe from high velocity dust hits, we urgently request the scientific community to obtain further measurements of the near-solar dust properties. One prime opportunity is the July 1991 solar eclipse.

scholarly journals The transition between long period comets, short period comets and meteoroid streams

1985 ◽  
Vol 83 ◽  
pp. 129-142
Author(s):  
David W. Hughes
Keyword(s):  
Solar System ◽  
Orbital Period ◽  
Maximum Rate ◽  
Meteoroid Stream ◽  
Meteoroid Streams ◽  
Long Period ◽  
Present Collection ◽  
Short Period ◽  
Comet Halley

It has long been realised that Jovian perturbation is the dominant cause of the transition of long period comets (Period > 200 yr) into short period ones (P < 200 yr). When the differences in the detectability of comets in the two groups are taken into account it is clear that the present day flux of long period comets is sufficient to provide the present collection of short period comets in the inner solar system.The fact that meteoroid streams are produced by decaying short period comets was first recognised around 1866 (see Hughes 1982a). The magnificent display of Leonids in that year enabled the radiant position and time of maximum rate to be easily calculated. Assuming the orbital period to be 33.25 yr Le Verrier (1867) and Schiaparelli (1867) published orbits for the meteoroid stream. The orbit of comet 1866 I, which had been discovered by Guillaume Tempel, from Marseilles on December 19, 1865 and independently by Horace P. Tuttle from Harvard, Massachusetts on January 5, 1866, has been calculated and published by Oppolzer (1867a). Almost to a man Peters (1867), Schiaparelli (1867) and Oppolzer (1867b) realised that the comet and the stream had similar orbits. Since that time many more examples have been put forward, two famous ones being the Perseids and comet Swift-Tuttle (1862 III) and the Eta Aquarids and Orionids both of which have comet Halley (1910 II) as their parent. For more details see Cook (1973).

scholarly journals In search of radio emission from exoplanets: GMRT observations of the binary system HD 41004

2020 ◽  
Vol 500 (4) ◽  
pp. 4818-4826
Author(s):  
Mayank Narang ◽  
P Manoj ◽  
C H Ishwara Chandra ◽  
Joseph Lazio ◽  
Thomas Henning ◽  
...  
Keyword(s):  
Binary System ◽  
Solar System ◽  
Magnetic Fields ◽  
Radio Emission ◽  
Radio Telescope ◽  
Orbital Period ◽  
Brown Dwarf ◽  
Primary Star ◽  
Strong Magnetic Fields

ABSTRACT This paper reports Giant Metrewave Radio Telescope (GMRT) observations of the binary system HD 41004 that are among the deepest images ever obtained at 150 and 400 MHz in the search for radio emission from exoplanets. The HD 41004 binary system consists of a K1 V primary star and an M2 V secondary; both stars are host to a massive planet or brown dwarf. Analogous to planets in our Solar system that emit at radio wavelengths due to their strong magnetic fields, one or both of the planet or brown dwarf in the HD 41004 binary system are also thought to be sources of radio emission. Various models predict HD 41004Bb to have one of the largest expected flux densities at 150 MHz. The observations at 150 MHz cover almost the entire orbital period of HD 41004Bb, and about $20{{\ \rm per\ cent}}$ of the orbit is covered at 400 MHz. We do not detect radio emission, setting 3σ limits of 1.8 mJy at 150 MHz and 0.12 mJy at 400 MHz. We also discuss some of the possible reasons why no radio emission was detected from the HD 41004 binary system.

scholarly journals On the Planetary Orbital Period Ratio Distribution In Multiple Planet Systems

2012 ◽  
Vol 8 (S293) ◽  
pp. 110-115
Author(s):  
Ji-Wei Xie
Keyword(s):  
Solar System ◽  
Orbital Period ◽  
Theoretical Models ◽  
Observational Constraints ◽  
Ratio Distribution ◽  
Period Ratio ◽  
First Order ◽  
Exact Resonance ◽  
Statistical Effect ◽  
Mission Period

AbstractMany multiple planet systems have been found by both radial velocity (RV) and transit surveys, such as the Kepler mission. Period ratio distribution of these planet candidates show that they do not prefer to be in or near Mean Motion Resonance (MMR). Nevertheless, there are small but significant excesses of candidate pairs both spaced slightly exterior to exact resonance, particular near the first order of MMR, such as 2:1 and 3:2. Here, we first review recent observational constraints on these multiple transiting systems and theoretical models, which attempt to understand their period ratio distributions. Then we identify a statistical effect based on an intrinsic asymmetry associated with MMR, and find it play an important role in shaping the period ratio distribution near MMR. Last but least, we also find such an intrinsic asymmetry is existing in asteroids of our solar system.

scholarly journals Dynamical masses of two infant giant planets

2021 ◽  
Author(s):  
Alejandro Suárez Mascareño ◽  
Mario Damasso ◽  
Nicolas Lodieu ◽  
Alessandro Sozzetti ◽  
Víctor Béjar ◽  
...  
Keyword(s):  
Solar System ◽  
Orbital Period ◽  
Giant Planets ◽  
Final Size ◽  
Stellar Activity ◽  
Planetary Evolution ◽  
Transiting Planets ◽  
Solar Type ◽  
Host Stars ◽  
Dynamical Masses

Abstract Current theories of planetary evolution predict that infant giant planets have large radii and very low densities before they slowly contract to reach their final size after about several hundred million years 1, 2. These theoretical expectations remain untested to date, despite the increasing number of exoplanetary discoveries, as the detection and characterisation of very young planets is extremely challenging due to the intense stellar activity of their host stars 3, 4. However, the recent discoveries of young planetary transiting systems allow to place initial constraints on evolutionary models5–9. With an estimated age of 20 million years, V1298 Tau is one of the youngest solar-type stars known to host transiting planets: it harbours a multiple system composed of two Neptune-sized, one Saturn-sized, and one Jupiter-sized planets 10, 11. Here we report the dynamical masses of two of the four planets. We find that planet b, with an orbital period of 24 days, has a mass of 0.60 Jupiter masses and a density similar to the giant planets of the Solar System and other known giant exoplanets with significantly older ages 12, 13. Planet e, with an orbital period of 40 days, has a mass of 1.21 Jupiter masses and a density larger than most giant exoplanets. This is unexpected for planets at such a young age and suggests that some giant planets might evolve and contract faster than anticipated, thus challenging current models of planetary evolution.

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