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The Cold Universe
Saas-Fee Advanced Course 32, 2002. Swiss Society for Astrophysics and Astronomy
Andrew W Blain, Francoise Combes, Bruce T Draine
€ 105,45
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Omschrijving
Modern astronomy has stretched its domains of exploration tremendously. Not only objects at very large distances and very old states of the Universe can be examined, but also all kinds of radiations and phenomena are now accessible. Astronomers constantly move from considerations about very - luted to very dense systems. Hot and energetic systems, being the easiest to observe, have attracted a lot of attention. However the cold and low energetic states have been so- what neglected, either because being harder to observe they appear unexc- ing, or because being less well known they tend to be ignored. However the Universe background radiation has now been determined as the most perfect known case of a black-body spectrum, a substantial fraction of matter spends some time close to the temperature of this universal thermal bath, before - ingtransformedintostarsorplanets. Someobjects, suchasrapidlyexpanding gas shells in planetary nebulae, may even succeed in reaching a temperature well below the background radiation temperature through the mere action of adiabatic expansion. In view of the highly dynamical and turbulent state of the interstellar medium, hot and cold temperature ?uctuations must be expected, while the clear observational bias is to observe the hot rather than the cold ?uctuations. Fortunately with the accessibility of far-infrared and sub-millimetric instruments such as SCUBA, WMAP, Planck or ALMA, we can expect in the coming years continuous advances in our understanding of these harder to observe cold stages of matter.
Specificaties
Betrokkenen
- Auteur(s):
- Uitgeverij:
Inhoud
- Aantal bladzijden:
- 310
- Taal:
- Engels
- Reeks:
- Reeksnummer:
- nr. 32
Eigenschappen
- Productcode (EAN):
- 9783540408383
- Verschijningsdatum:
- 17/10/2003
- Uitvoering:
- Hardcover
- Formaat:
- Genaaid
- Afmetingen:
- 156 mm x 234 mm
- Gewicht:
- 625 g
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