Optimal spacecraft asymptotic velocity for the high inclined orbits formation using gravity assists in the planetary systems

An adaptive, semi‑analytical, and geometrically clear method for synthesis of sequences of Venusian gravity‑assist maneuvers setting the desired inclination of a spacecraft orbit is proposed. The geometric constraint on the maximum possible inclination of a spacecraft orbit, which depends on the asymptotic spacecraft velocity relative to Venus, and the dynamic constraint (arising when a gravity‑assist maneuver is performed) on the angle of rotation of the vector of asymptotic velocity relative to Venus are considered simultaneously.

Download Full-text

Dust in the Solar System and other Planetary Systems, Proceedings of the IA U Colloquium 181 held at the University of Kent

10.1016/s0964-2749(02)x8242-0 ◽

2002 ◽

Keyword(s):

Solar System ◽

Planetary Systems ◽

The University

Download Full-text

From Dust to Life

10.23943/princeton/9780691175706.001.0001 ◽

2017 ◽

Author(s):

John Chambers ◽

Jacqueline Mitton

Keyword(s):

Solar System ◽

Extrasolar Planets ◽

Planetary Systems ◽

History Of Astronomy ◽

Human Origins ◽

History Of ◽

The Subject ◽

Emergence Of Life

The birth and evolution of our solar system is a tantalizing mystery that may one day provide answers to the question of human origins. This book tells the remarkable story of how the celestial objects that make up the solar system arose from common beginnings billions of years ago, and how scientists and philosophers have sought to unravel this mystery down through the centuries, piecing together the clues that enabled them to deduce the solar system's layout, its age, and the most likely way it formed. Drawing on the history of astronomy and the latest findings in astrophysics and the planetary sciences, the book offers the most up-to-date and authoritative treatment of the subject available. It examines how the evolving universe set the stage for the appearance of our Sun, and how the nebulous cloud of gas and dust that accompanied the young Sun eventually became the planets, comets, moons, and asteroids that exist today. It explores how each of the planets acquired its unique characteristics, why some are rocky and others gaseous, and why one planet in particular—our Earth—provided an almost perfect haven for the emergence of life. The book takes readers to the very frontiers of modern research, engaging with the latest controversies and debates. It reveals how ongoing discoveries of far-distant extrasolar planets and planetary systems are transforming our understanding of our own solar system's astonishing history and its possible fate.

Download Full-text

Generation of Unbound Comets and Planets by Planetary Systems

Astronomy Reports ◽

10.1134/s1063772920110098 ◽

2020 ◽

Vol 64 (11) ◽

pp. 936-949

Author(s):

A. V. Tutukov ◽

G. N. Dremova ◽

V. V. Dremov

Keyword(s):

Planetary Systems

Download Full-text

Exploring the Solar System

10.1093/oso/9780198799894.003.0003 ◽

2018 ◽

Author(s):

Karel Schrijver

Keyword(s):

Solar System ◽

Planetary Systems ◽

Interplanetary Dust ◽

Terrestrial Planets ◽

The Moon ◽

System P ◽

Asteroids And Comets

In this chapter, the author summarizes the properties of the Solar System, and how these were uncovered. Over centuries, the arrangement and properties of the Solar System were determined. The distinctions between the terrestrial planets, the gas and ice giants, and their various moons are discussed. Whereas humans have walked only on the Moon, probes have visited all the planets and several moons, asteroids, and comets; samples have been returned to Earth only from our moon, a comet, and from interplanetary dust. For Earth and Moon, seismographs probed their interior, whereas for other planets insights come from spacecraft and meteorites. We learned that elements separated between planet cores and mantels because larger bodies in the Solar System were once liquid, and many still are. How water ended up where it is presents a complex puzzle. Will the characteristics of our Solar System hold true for planetary systems in general?

Download Full-text

The Long View of Planetary Systems

10.1093/oso/9780198799894.003.0011 ◽

2018 ◽

Author(s):

Karel Schrijver

Keyword(s):

Solar System ◽

Milky Way ◽

Planetary Systems ◽

Giant Planets ◽

Milky Way Galaxy ◽

Population Statistics ◽

The Past ◽

General Terms ◽

The Galaxy ◽

The Universe

How many planetary systems formed before our’s did, and how many will form after? How old is the average exoplanet in the Galaxy? When did the earliest planets start forming? How different are the ages of terrestrial and giant planets? And, ultimately, what will the fate be of our Solar System, of the Milky Way Galaxy, and of the Universe around us? We cannot know the fate of individual exoplanets with great certainty, but based on population statistics this chapter sketches the past, present, and future of exoworlds and of our Earth in general terms.

Download Full-text

Asymptotic velocity of relativistic E × B drift

AIP Advances ◽

10.1063/5.0029013 ◽

2021 ◽

Vol 11 (3) ◽

pp. 035303

Author(s):

Tatsufumi Nakamura

Keyword(s):

Asymptotic Velocity

Download Full-text

Double trouble: Gaia reveals (proto)planetary systems that may experience more than one dense star-forming environment

Monthly Notices of the Royal Astronomical Society Letters ◽

10.1093/mnrasl/slaa182 ◽

2020 ◽

Vol 501 (1) ◽

pp. L12-L17

Author(s):

Christina Schoettler ◽

Richard J Parker

Keyword(s):

Planetary Systems ◽

Young Star ◽

Young Stars ◽

Orion Nebula ◽

External Effects ◽

Star Forming ◽

Star Forming Regions ◽

Ejection Process ◽

Runaway Stars

ABSTRACT Planetary systems appear to form contemporaneously around young stars within young star-forming regions. Within these environments, the chances of survival, as well as the long-term evolution of these systems, are influenced by factors such as dynamical interactions with other stars and photoevaporation from massive stars. These interactions can also cause young stars to be ejected from their birth regions and become runaways. We present examples of such runaway stars in the vicinity of the Orion Nebula Cluster (ONC) found in Gaia DR2 data that have retained their discs during the ejection process. Once set on their path, these runaways usually do not encounter any other dense regions that could endanger the survival of their discs or young planetary systems. However, we show that it is possible for star–disc systems, presumably ejected from one dense star-forming region, to encounter a second dense region, in our case the ONC. While the interactions of the ejected star–disc systems in the second region are unlikely to be the same as in their birth region, a second encounter will increase the risk to the disc or planetary system from malign external effects.

Download Full-text

DESTINY: Database for the Effects of STellar encounters on dIsks and plaNetary sYstems

Computational Astrophysics and Cosmology ◽

10.1186/s40668-019-0030-3 ◽

2019 ◽

Vol 6 (1) ◽

Cited By ~ 2

Author(s):

Asmita Bhandare ◽

Susanne Pfalzner

Keyword(s):

Planetary System ◽

Planetary Systems ◽

Gravitational Effect ◽

Parameter Study ◽

Orbital Inclination ◽

Particle Properties ◽

Disk Size ◽

Stellar Group ◽

Cluster Environment ◽

Parabolic Orbits

Abstract Most stars form as part of a stellar group. These young stars are mostly surrounded by a disk from which potentially a planetary system might form. Both, the disk and later on the planetary system, may be affected by the cluster environment due to close fly-bys. The here presented database can be used to determine the gravitational effect of such fly-bys on non-viscous disks and planetary systems. The database contains data for fly-by scenarios spanning mass ratios between the perturber and host star from 0.3 to 50.0, periastron distances from 30 au to 1000 au, orbital inclination from 0∘ to 180∘ and angle of periastron of 0∘, 45∘ and 90∘. Thus covering a wide parameter space relevant for fly-bys in stellar clusters. The data can either be downloaded to perform one’s own diagnostics like for e.g. determining disk size, disk mass, etc. after specific encounters, obtain parameter dependencies or the different particle properties can be visualized interactively. Currently the database is restricted to fly-bys on parabolic orbits, but it will be extended to hyperbolic orbits in the future. All of the data from this extensive parameter study is now publicly available as DESTINY.

Download Full-text