Exoplanets: Detection, Formation, Properties, Habitability (Springer Praxis Books)
Language: English
Pages: 328
ISBN: 3642093280
Format: PDF / Kindle (mobi) / ePub
This is the first collection of review articles in one volume covering the very latest developments in exoplanet research. This edited, multi-author volume will be an invaluable introduction and reference to all key aspects in the field this field. The reviews cover topics such as the properties of known exoplanets and searching for exoplanets in the stellar graveyard. The book provides an easily accessible point of reference in a fast moving and exciting field.
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its star, is calculated to be enormous (∼ 1400 K) and the planet has been dubbed a ‘hot Jupiter’. 1.2 Detection of Extrasolar Planets Directly observing extrasolar planets is extremely difficult given the large brightness contrast between a star and its planets and also the small angular separation. For 2 Patrick G. J. Irwin example, if our own Solar System were observed at a distance of, say, 5 parsecs, the greatest angular separation of the Sun and Jupiter would be just 1 arcsecond with the
the radius where solartype stars collect. Further data is required in order to robustly test this hypothesis, e.g., Fig. 6.9. The rise in the number of exoplanets towards longer periods is becoming more apparent as more planets are discovered and is very well reproduced by exoplanet migration scenarios which envisage planets migrating inwards (e.g., Armitage et al. 2002; Trilling et al. 2003) as well as outwards (Masset & Papaloizou 2003). 6.5.1 Planet Formation The favoured model of forming the
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will occur, but if the velocities are low there is a high probability the grains will stick and cause the boulders to grow. In addition, the boulders will lose orbital energy to the headwind and spiral in toward the star, eventually evaporating. The smaller boulders may have to grow rapidly to survive, since the gas headwind becomes more effective with the decreasing volume to surface area ratio of smaller objects. The difficulties in gradual growth while avoiding spiralling inward too close to the
disk does have observable consequences. Indeed, there are likely to be fewer ambiguities under this classification system than relying on an arbitrary, and essentially unmeasureable, mass limit that applies to all very lowmass objects. Moreover, identifying isolated < 0.013M objects as ”planets” or even ”exoplanets” is likely to add further unnecessary post-Pluto confusion about that term among the lay public. We prefer to preserve the traditional terminology, and distinguish brown dwarfs and
