A CORRELATION BETWEEN HOST STAR ACTIVITY AND PLANET MASS FOR CLOSE-IN EXTRASOLAR PLANETS?

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.

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Parent Stars of Extrasolar Planets. V. HD 75289

The Astronomical Journal ◽

10.1086/301176 ◽

2000 ◽

Vol 119 (1) ◽

pp. 390-396 ◽

Cited By ~ 101

Author(s):

Guillermo Gonzalez ◽

Chris Laws

Keyword(s):

Extrasolar Planets

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MODELING THE INFRARED SPECTRUM OF THE EARTH-MOON SYSTEM: IMPLICATIONS FOR THE DETECTION AND CHARACTERIZATION OF EARTHLIKE EXTRASOLAR PLANETS AND THEIR MOONLIKE COMPANIONS

The Astrophysical Journal ◽

10.1088/0004-637x/741/1/51 ◽

2011 ◽

Vol 741 (1) ◽

pp. 51 ◽

Cited By ~ 23

Author(s):

Tyler D. Robinson

Keyword(s):

Infrared Spectrum ◽

Extrasolar Planets ◽

Moon System ◽

The Earth

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Phase transitions beyond post-perovskite in NaMgF3 to 160 GPa

Proceedings of the National Academy of Sciences ◽

10.1073/pnas.1909446116 ◽

2019 ◽

Vol 116 (39) ◽

pp. 19324-19329 ◽

Cited By ~ 1

Author(s):

Rajkrishna Dutta ◽

Eran Greenberg ◽

Vitali B. Prakapenka ◽

Thomas S. Duffy

Keyword(s):

Phase Transitions ◽

Diamond Anvil Cell ◽

Extrasolar Planets ◽

High Pressures ◽

Model System ◽

Similar Sequence ◽

Deep Interior ◽

Diamond Anvil ◽

Binary Compounds ◽

Pressure Phase

Neighborite, NaMgF3, is used as a model system for understanding phase transitions in ABX3 systems (e.g., MgSiO3) at high pressures. Here we report diamond anvil cell experiments that identify the following phases in NaMgF3 with compression to 162 GPa: NaMgF3 (perovskite) → NaMgF3 (post-perovskite) → NaMgF3 (Sb2S3-type) → NaF (B2-type) + NaMg2F5 (P21/c) → NaF (B2) + MgF2 (cotunnite-type). Our results demonstrate the existence of an Sb2S3-type post-post-perovskite ABX3 phase. We also experimentally demonstrate the formation of the P21/c AB2X5 phase which has been proposed theoretically to be a common high-pressure phase in ABX3 systems. Our study provides an experimental observation of the full sequence of phase transitions from perovskite to post-perovskite to post-post-perovskite followed by 2-stage breakdown to binary compounds. Notably, a similar sequence of transitions is predicted to occur in MgSiO3 at ultrahigh pressures, where it has implications for the mineralogy and dynamics in the deep interior of large, rocky extrasolar planets.

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Asteroid collisions as origin of debris disks: Asteroid shape reconstruction from BNAO Rozhen photometry

Proceedings of the International Astronomical Union ◽

10.1017/s1743921319009426 ◽

2019 ◽

Vol 15 (S350) ◽

pp. 451-453

Author(s):

G. Apostolovska ◽

E. Vchkova Bebekovska ◽

A. Kostov ◽

Z. Donchev

Keyword(s):

Laboratory Experiments ◽

Extrasolar Planets ◽

Shape Reconstruction ◽

Inversion Method ◽

Debris Disks ◽

Shape Parameters ◽

Zodiacal Cloud ◽

Photometric Observations ◽

Different Shapes ◽

Asteroid Surface

AbstractAs a result of collisions during their lifetimes, asteroids have a large variety of different shapes. It is believed that high velocity collisions or rotational spin-up of asteroids continuously replenish the Sun’s zodiacal cloud and debris disks around extrasolar planets (Jewitt (2010)). Knowledge of the spin and shape parameters of the asteroids is very important for understanding collision asteroid processes. Lately photometric observations of asteroids showed that variations in brightness are not accompanied by variations in colour index which indicate that the shape of the lightcurve is caused by varying illuminations of the asteroid surface rather than albedo variations over the surface. This conclusion became possible when photometric investigations were combined with laboratory experiments (Dunlap (1971)). In this article using the convex lightcurve inversion method we obtained the sense of rotation, pole solutions and preliminary shape of 901 Brunsia.

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