Bohringer Hans (Over 1,000 results)

Taschenbuch. Condition: Gut. 169 S. Das hier angebotene Buch stammt aus einer teilaufgelösten Bibliothek und kann die entsprechenden Kennzeichnungen aufweisen (Rückenschild, Instituts-Stempel.); der Buchzustand ist ansonsten ordentlich und dem Alter entsprechend gut. Sprache: Deutsch Gewicht in Gramm: 220.…

Taschenbuch. Condition: Gut. 50 Seiten; Das Taschenbuch stammt aus einer Bibliotheksauflösung. Instituts-Stempel. Sprache: Deutsch Gewicht in Gramm: 100.

Taschenbuch. Condition: Gut. 50 Seiten, Das Buch ist ordentlich erhalten und kann altersbedingte Gebrauchsspuren aufweisen. Sprache: Deutsch Gewicht in Gramm: 150.

Hardcover. Condition: Wie neu. XXIII, 444 S. : Ill. Like new. Shrink wrapped. Sprache: Englisch Gewicht in Gramm: 915.

Condition: New. This is a Brand-new US Edition. This Item may be shipped from US or any other country as we have multiple locations worldwide.

Condition: Brand New. New. US edition. Expediting shipping for all USA and Europe orders excluding PO Box. Excellent Customer Service.

Condition: New. Brand New Original US Edition. Customer service! Satisfaction Guaranteed.

Condition: New. pp. xxiv + 446 1st Edition.

paperback. Condition: As New. Softcover. Good binding and cover. Clean, unmarked pages. 728 pages Annals of the NY Academy of Science vol. 759.

Condition: New. pp. xxiv + 446.

large paperbac. 728 pages VG++ Annals of the NY Academy of Science Volume 759, very scarce.

Softcover, Heft. 20 Seiten Die Jahresangabe ist ungefähr. Zustand: keine Beschädigungen, eine Eintragung auf letzter Seite. Rücken, Ecken, Kanten gut. Sprache: Deutsch Gewicht in Gramm: 200.

8°, Broschiert. Einige s/w Abb., 728 S.; Text in engl. Spr., Einb. und Kanten gering bestoßen, ansonsten kaum Gebrauchsspuren vorhanden, gutes Exemplar Sprache: Englisch Gewicht in Gramm: 1500.

Original-Broschur, mit 1 ausfaltb. Karte, 91 Seiten, 15,5 x 23 cm, gut erhalten.

gr. 8° - 496 S. illustr. OPpbd., 2 CD-Roms (ungeöffnet), sehr gutes, frisches Exemplar, ohne Einträge. Die angegebenen Versandkosten können von den tatsächlichen Versandkosten (z.B. aufgrund höheren Gewichts) abweichen. The stated shipping costs may differ from the actual shipping costs (e.g. due to higher weight). Sprache: Deutsch 1420 gr.…

212 S., zahlr. Abb., gr.okt., ill. Pp., SchU., (2) mehrf. gef. Ktn.- [ Landeskunde Geschichte DE707 Zeit1229 -Zeit1979 J| 1979 N| Wilfried Setzler N| Dieter Böhringer N| Herbert Bühler N| Rainer Häußler N| Lothar Reinhard N| Hans Georg Hofacker | 89697 ].

Softcover. 65 Seiten Nur Nr. 82. Zustand: Keine Beschädigungen, mit einer Namenseintragung im Vorsatz. Rücken, Ecken, Kanten gut. Mit einem zusätzlichen Folieneinband (keine Klebefolie). Sprache: Deutsch Gewicht in Gramm: 150.

Condition: New. In.

Condition: New.

Taschenbuch. o.A. 50 S. Leichte Lager- und Gebrauchsspuren. Ausgeschiedenes Bibliotheksexemplar mit den üblichen Kennzeichnungen, Einband leicht verschmutzt. Ansonsten innen wie außen ein sehr gutes Exemplar. Die Leseseiten sind sauber und ohne Anstreichungen oder Knicke. Sprache: Deutsch Gewicht in Gramm: 200.…

Condition: New.

Condition: New. pp. 472.

Buch. Condition: Neu. Druck auf Anfrage Neuware - Printed after ordering - The Universe would be a dull and dark place if the gaseous baryons did not cool, collapse, and form stars and galaxies. However, if this gas is allowed to cool unimpeded at the rate predicted from known atomic physics, in the context of a well-established cosmological model, the gaseous matter would form stars and galaxies with a high e ciency, so that far more than the observed fraction of about 10-15% of the baryonic matter would be found in luminous stellar systems. Therefore,cooling must be damped or regulatedby heating processes, and observations show that this 'feedback' is a widespread astrophysical phenomenon. The place where this cooling and feedback manifests itself most dram- ically is in the inner regions of the most massive Dark Matter halos found in our Universe, in the cores of galaxy clusters. The e ect of cosmic co- ing in these objects was recognized in the mid-1970s, and the term 'cooling ow' was introduced by Andy Fabian and colleagues at Cambridge as a p- sible explanation of the physical processes obtained in the central regions of clusters. The name refers to the fact that gas cooling in the inner regions is associated with a loss of central pressure, causing an in ow of hot gas from larger radii.…

Hardcover. Condition: New Books. Brand New! Fast Delivery This is an International Edition and ship within 24-48 hours. Deliver by FedEx and Dhl, & Aramex, UPS, & USPS and we do accept APO and PO BOX Addresses. Order can be delivered worldwide within 6-10 days and we do have flat rate for up to 2LB. Extra shipping charges will be requested if the Book weight is more than 5 LB. This Item May be shipped from India, United states & United Kingdom. Depending on your location and availability. …

Taschenbuch. Condition: Neu. Druck auf Anfrage Neuware - Printed after ordering - The Universe would be a dull and dark place if the gaseous baryons did not cool, collapse, and form stars and galaxies. However, if this gas is allowed to cool unimpeded at the rate predicted from known atomic physics, in the context of a well-established cosmological model, the gaseous matter would form stars and galaxies with a high e ciency, so that far more than the observed fraction of about 10-15% of the baryonic matter would be found in luminous stellar systems. Therefore,cooling must be damped or regulatedby heating processes, and observations show that this 'feedback' is a widespread astrophysical phenomenon. The place where this cooling and feedback manifests itself most dram- ically is in the inner regions of the most massive Dark Matter halos found in our Universe, in the cores of galaxy clusters. The e ect of cosmic co- ing in these objects was recognized in the mid-1970s, and the term 'cooling ow' was introduced by Andy Fabian and colleagues at Cambridge as a p- sible explanation of the physical processes obtained in the central regions of clusters. The name refers to the fact that gas cooling in the inner regions is associated with a loss of central pressure, causing an in ow of hot gas from larger radii. …

Taschenbuch. Condition: Neu. Heating versus Cooling in Galaxies and Clusters of Galaxies | Proceedings of the MPA/ESO/MPE/USM Joint Astronomy Conference held in Garching, Germany, 6-11 August 2006 | Hans Böhringer (u. a.) | Taschenbuch | xxiii | Englisch | 2010 | Springer | EAN 9783642092572 | Verantwortliche Person für die EU: Springer Verlag GmbH, Tiergartenstr. 17, 69121 Heidelberg, juergen[dot]hartmann[at]springer[dot]com | Anbieter: preigu.…

Condition: Sehr gut. Zustand: Sehr gut | Seiten: 472 | Sprache: Englisch | Produktart: Bücher | The Universe would be a dull and dark place if the gaseous baryons did not cool, collapse, and form stars and galaxies. However, if this gas is allowed to cool unimpeded at the rate predicted from known atomic physics, in the context of a well-established cosmological model, the gaseous matter would form stars and galaxies with a high e?ciency, so that far more than the observed fraction of about 10¿15% of the baryonic matter would be found in luminous stellar systems. Therefore,cooling must be damped or regulatedby heating processes, and observations show that this ¿feedback¿ is a widespread astrophysical phenomenon. The place where this cooling and feedback manifests itself most dram- ically is in the inner regions of the most massive Dark Matter halos found in our Universe, in the cores of galaxy clusters. The e?ect of cosmic co- ing in these objects was recognized in the mid-1970s, and the term ¿cooling ?ow¿ was introduced by Andy Fabian and colleagues at Cambridge as a p- sible explanation of the physical processes obtained in the central regions of clusters. The name refers to the fact that gas cooling in the inner regions is associated with a loss of central pressure, causing an in?ow of hot gas from larger radii.…

Condition: New. In.

Paperback. Condition: New.

Condition: As New. Unread book in perfect condition.