Cooling Flows in Clusters and Galaxies:
Gespeichert in:
| 1. Verfasser: | |
|---|---|
| Format: | Elektronisch E-Book |
| Sprache: | English |
| Veröffentlicht: |
Dordrecht
Springer Netherlands
1988
|
| Schriftenreihe: | NATO ASI Series, Series C: Mathematical and Physical Sciences
229 |
| Schlagworte: | |
| Online-Zugang: | Volltext |
| Beschreibung: | X-ray astronomers discovered the diffuse gas in clusters of galaxies about 20 years ago. It was later realized that the central gas density in some clusters, and in elliptical galaxies, is so high that radiative cooling is a significant energy loss. The cooling time of the gas decreases rapidly towards the centre of the cluster or galaxy and is less than a Hubble time within the innermost few hundred kiloparsecs. This results in a cooling flow in which the gas density rises in order to maintain pressure to support the weight of the overlying gas. The rate at which mass is deposited by the flow is inferred to be several hundreds of solar masses per year in some clusters. The fraction of clusters in which cooling flows are found may exceed 50 per cent. Small flows probably occur in most normal elliptical galaxies that are not in rich clusters. The implications of this simple phenomenon are profound, for we appear to be witnessing the ongoing formation of the central galaxy. In particular, since most of the gas is undetected once it cools below about 3 million K, it appears to form dark matter. There is no reason why it should be detectable with current techniques if each cooling proton only recombines once and the matter condenses into objects of low mass |
| Beschreibung: | 1 Online-Ressource (406p) |
| ISBN: | 9789400929531 9789401078283 |
| ISSN: | 1389-2185 |
| DOI: | 10.1007/978-94-009-2953-1 |
Internformat
MARC
| LEADER | 00000nmm a2200000zcb4500 | ||
|---|---|---|---|
| 001 | BV042415054 | ||
| 003 | DE-604 | ||
| 005 | 00000000000000.0 | ||
| 007 | cr|uuu---uuuuu | ||
| 008 | 150316s1988 |||| o||u| ||||||eng d | ||
| 020 | |a 9789400929531 |c Online |9 978-94-009-2953-1 | ||
| 020 | |a 9789401078283 |c Print |9 978-94-010-7828-3 | ||
| 024 | 7 | |a 10.1007/978-94-009-2953-1 |2 doi | |
| 035 | |a (OCoLC)863785092 | ||
| 035 | |a (DE-599)BVBBV042415054 | ||
| 040 | |a DE-604 |b ger |e aacr | ||
| 041 | 0 | |a eng | |
| 049 | |a DE-91 |a DE-83 | ||
| 082 | 0 | |a 520 |2 23 | |
| 084 | |a PHY 000 |2 stub | ||
| 100 | 1 | |a Fabian, A. C. |e Verfasser |4 aut | |
| 245 | 1 | 0 | |a Cooling Flows in Clusters and Galaxies |c edited by A. C. Fabian |
| 246 | 1 | 3 | |a Proceedings of the NATO Advanced Research Workshop, Cambridge, U.K., June 22-26, 1987 |
| 264 | 1 | |a Dordrecht |b Springer Netherlands |c 1988 | |
| 300 | |a 1 Online-Ressource (406p) | ||
| 336 | |b txt |2 rdacontent | ||
| 337 | |b c |2 rdamedia | ||
| 338 | |b cr |2 rdacarrier | ||
| 490 | 0 | |a NATO ASI Series, Series C: Mathematical and Physical Sciences |v 229 |x 1389-2185 | |
| 500 | |a X-ray astronomers discovered the diffuse gas in clusters of galaxies about 20 years ago. It was later realized that the central gas density in some clusters, and in elliptical galaxies, is so high that radiative cooling is a significant energy loss. The cooling time of the gas decreases rapidly towards the centre of the cluster or galaxy and is less than a Hubble time within the innermost few hundred kiloparsecs. This results in a cooling flow in which the gas density rises in order to maintain pressure to support the weight of the overlying gas. The rate at which mass is deposited by the flow is inferred to be several hundreds of solar masses per year in some clusters. The fraction of clusters in which cooling flows are found may exceed 50 per cent. Small flows probably occur in most normal elliptical galaxies that are not in rich clusters. The implications of this simple phenomenon are profound, for we appear to be witnessing the ongoing formation of the central galaxy. In particular, since most of the gas is undetected once it cools below about 3 million K, it appears to form dark matter. There is no reason why it should be detectable with current techniques if each cooling proton only recombines once and the matter condenses into objects of low mass | ||
| 650 | 4 | |a Physics | |
| 650 | 4 | |a Astronomy, Observations and Techniques | |
| 650 | 0 | 7 | |a Gasströmung |0 (DE-588)4156052-8 |2 gnd |9 rswk-swf |
| 650 | 0 | 7 | |a Interstellares Gas |0 (DE-588)4162147-5 |2 gnd |9 rswk-swf |
| 655 | 7 | |8 1\p |0 (DE-588)1071861417 |a Konferenzschrift |y 1987 |z Cambridge |2 gnd-content | |
| 689 | 0 | 0 | |a Interstellares Gas |0 (DE-588)4162147-5 |D s |
| 689 | 0 | 1 | |a Gasströmung |0 (DE-588)4156052-8 |D s |
| 689 | 0 | |8 2\p |5 DE-604 | |
| 856 | 4 | 0 | |u https://doi.org/10.1007/978-94-009-2953-1 |x Verlag |3 Volltext |
| 912 | |a ZDB-2-PHA |a ZDB-2-BAE | ||
| 940 | 1 | |q ZDB-2-PHA_Archive | |
| 999 | |a oai:aleph.bib-bvb.de:BVB01-027850547 | ||
| 883 | 1 | |8 1\p |a cgwrk |d 20201028 |q DE-101 |u https://d-nb.info/provenance/plan#cgwrk | |
| 883 | 1 | |8 2\p |a cgwrk |d 20201028 |q DE-101 |u https://d-nb.info/provenance/plan#cgwrk | |
Datensatz im Suchindex
| _version_ | 1804153081626099712 |
|---|---|
| any_adam_object | |
| author | Fabian, A. C. |
| author_facet | Fabian, A. C. |
| author_role | aut |
| author_sort | Fabian, A. C. |
| author_variant | a c f ac acf |
| building | Verbundindex |
| bvnumber | BV042415054 |
| classification_tum | PHY 000 |
| collection | ZDB-2-PHA ZDB-2-BAE |
| ctrlnum | (OCoLC)863785092 (DE-599)BVBBV042415054 |
| dewey-full | 520 |
| dewey-hundreds | 500 - Natural sciences and mathematics |
| dewey-ones | 520 - Astronomy and allied sciences |
| dewey-raw | 520 |
| dewey-search | 520 |
| dewey-sort | 3520 |
| dewey-tens | 520 - Astronomy and allied sciences |
| discipline | Physik |
| doi_str_mv | 10.1007/978-94-009-2953-1 |
| format | Electronic eBook |
| fullrecord | <?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>03152nmm a2200493zcb4500</leader><controlfield tag="001">BV042415054</controlfield><controlfield tag="003">DE-604</controlfield><controlfield tag="005">00000000000000.0</controlfield><controlfield tag="007">cr|uuu---uuuuu</controlfield><controlfield tag="008">150316s1988 |||| o||u| ||||||eng d</controlfield><datafield tag="020" ind1=" " ind2=" "><subfield code="a">9789400929531</subfield><subfield code="c">Online</subfield><subfield code="9">978-94-009-2953-1</subfield></datafield><datafield tag="020" ind1=" " ind2=" "><subfield code="a">9789401078283</subfield><subfield code="c">Print</subfield><subfield code="9">978-94-010-7828-3</subfield></datafield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1007/978-94-009-2953-1</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(OCoLC)863785092</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-599)BVBBV042415054</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-604</subfield><subfield code="b">ger</subfield><subfield code="e">aacr</subfield></datafield><datafield tag="041" ind1="0" ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="049" ind1=" " ind2=" "><subfield code="a">DE-91</subfield><subfield code="a">DE-83</subfield></datafield><datafield tag="082" ind1="0" ind2=" "><subfield code="a">520</subfield><subfield code="2">23</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">PHY 000</subfield><subfield code="2">stub</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Fabian, A. C.</subfield><subfield code="e">Verfasser</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Cooling Flows in Clusters and Galaxies</subfield><subfield code="c">edited by A. C. Fabian</subfield></datafield><datafield tag="246" ind1="1" ind2="3"><subfield code="a">Proceedings of the NATO Advanced Research Workshop, Cambridge, U.K., June 22-26, 1987</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="a">Dordrecht</subfield><subfield code="b">Springer Netherlands</subfield><subfield code="c">1988</subfield></datafield><datafield tag="300" ind1=" " ind2=" "><subfield code="a">1 Online-Ressource (406p)</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="490" ind1="0" ind2=" "><subfield code="a">NATO ASI Series, Series C: Mathematical and Physical Sciences</subfield><subfield code="v">229</subfield><subfield code="x">1389-2185</subfield></datafield><datafield tag="500" ind1=" " ind2=" "><subfield code="a">X-ray astronomers discovered the diffuse gas in clusters of galaxies about 20 years ago. It was later realized that the central gas density in some clusters, and in elliptical galaxies, is so high that radiative cooling is a significant energy loss. The cooling time of the gas decreases rapidly towards the centre of the cluster or galaxy and is less than a Hubble time within the innermost few hundred kiloparsecs. This results in a cooling flow in which the gas density rises in order to maintain pressure to support the weight of the overlying gas. The rate at which mass is deposited by the flow is inferred to be several hundreds of solar masses per year in some clusters. The fraction of clusters in which cooling flows are found may exceed 50 per cent. Small flows probably occur in most normal elliptical galaxies that are not in rich clusters. The implications of this simple phenomenon are profound, for we appear to be witnessing the ongoing formation of the central galaxy. In particular, since most of the gas is undetected once it cools below about 3 million K, it appears to form dark matter. There is no reason why it should be detectable with current techniques if each cooling proton only recombines once and the matter condenses into objects of low mass</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Physics</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Astronomy, Observations and Techniques</subfield></datafield><datafield tag="650" ind1="0" ind2="7"><subfield code="a">Gasströmung</subfield><subfield code="0">(DE-588)4156052-8</subfield><subfield code="2">gnd</subfield><subfield code="9">rswk-swf</subfield></datafield><datafield tag="650" ind1="0" ind2="7"><subfield code="a">Interstellares Gas</subfield><subfield code="0">(DE-588)4162147-5</subfield><subfield code="2">gnd</subfield><subfield code="9">rswk-swf</subfield></datafield><datafield tag="655" ind1=" " ind2="7"><subfield code="8">1\p</subfield><subfield code="0">(DE-588)1071861417</subfield><subfield code="a">Konferenzschrift</subfield><subfield code="y">1987</subfield><subfield code="z">Cambridge</subfield><subfield code="2">gnd-content</subfield></datafield><datafield tag="689" ind1="0" ind2="0"><subfield code="a">Interstellares Gas</subfield><subfield code="0">(DE-588)4162147-5</subfield><subfield code="D">s</subfield></datafield><datafield tag="689" ind1="0" ind2="1"><subfield code="a">Gasströmung</subfield><subfield code="0">(DE-588)4156052-8</subfield><subfield code="D">s</subfield></datafield><datafield tag="689" ind1="0" ind2=" "><subfield code="8">2\p</subfield><subfield code="5">DE-604</subfield></datafield><datafield tag="856" ind1="4" ind2="0"><subfield code="u">https://doi.org/10.1007/978-94-009-2953-1</subfield><subfield code="x">Verlag</subfield><subfield code="3">Volltext</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">ZDB-2-PHA</subfield><subfield code="a">ZDB-2-BAE</subfield></datafield><datafield tag="940" ind1="1" ind2=" "><subfield code="q">ZDB-2-PHA_Archive</subfield></datafield><datafield tag="999" ind1=" " ind2=" "><subfield code="a">oai:aleph.bib-bvb.de:BVB01-027850547</subfield></datafield><datafield tag="883" ind1="1" ind2=" "><subfield code="8">1\p</subfield><subfield code="a">cgwrk</subfield><subfield code="d">20201028</subfield><subfield code="q">DE-101</subfield><subfield code="u">https://d-nb.info/provenance/plan#cgwrk</subfield></datafield><datafield tag="883" ind1="1" ind2=" "><subfield code="8">2\p</subfield><subfield code="a">cgwrk</subfield><subfield code="d">20201028</subfield><subfield code="q">DE-101</subfield><subfield code="u">https://d-nb.info/provenance/plan#cgwrk</subfield></datafield></record></collection> |
| genre | 1\p (DE-588)1071861417 Konferenzschrift 1987 Cambridge gnd-content |
| genre_facet | Konferenzschrift 1987 Cambridge |
| id | DE-604.BV042415054 |
| illustrated | Not Illustrated |
| indexdate | 2024-07-10T01:20:56Z |
| institution | BVB |
| isbn | 9789400929531 9789401078283 |
| issn | 1389-2185 |
| language | English |
| oai_aleph_id | oai:aleph.bib-bvb.de:BVB01-027850547 |
| oclc_num | 863785092 |
| open_access_boolean | |
| owner | DE-91 DE-BY-TUM DE-83 |
| owner_facet | DE-91 DE-BY-TUM DE-83 |
| physical | 1 Online-Ressource (406p) |
| psigel | ZDB-2-PHA ZDB-2-BAE ZDB-2-PHA_Archive |
| publishDate | 1988 |
| publishDateSearch | 1988 |
| publishDateSort | 1988 |
| publisher | Springer Netherlands |
| record_format | marc |
| series2 | NATO ASI Series, Series C: Mathematical and Physical Sciences |
| spelling | Fabian, A. C. Verfasser aut Cooling Flows in Clusters and Galaxies edited by A. C. Fabian Proceedings of the NATO Advanced Research Workshop, Cambridge, U.K., June 22-26, 1987 Dordrecht Springer Netherlands 1988 1 Online-Ressource (406p) txt rdacontent c rdamedia cr rdacarrier NATO ASI Series, Series C: Mathematical and Physical Sciences 229 1389-2185 X-ray astronomers discovered the diffuse gas in clusters of galaxies about 20 years ago. It was later realized that the central gas density in some clusters, and in elliptical galaxies, is so high that radiative cooling is a significant energy loss. The cooling time of the gas decreases rapidly towards the centre of the cluster or galaxy and is less than a Hubble time within the innermost few hundred kiloparsecs. This results in a cooling flow in which the gas density rises in order to maintain pressure to support the weight of the overlying gas. The rate at which mass is deposited by the flow is inferred to be several hundreds of solar masses per year in some clusters. The fraction of clusters in which cooling flows are found may exceed 50 per cent. Small flows probably occur in most normal elliptical galaxies that are not in rich clusters. The implications of this simple phenomenon are profound, for we appear to be witnessing the ongoing formation of the central galaxy. In particular, since most of the gas is undetected once it cools below about 3 million K, it appears to form dark matter. There is no reason why it should be detectable with current techniques if each cooling proton only recombines once and the matter condenses into objects of low mass Physics Astronomy, Observations and Techniques Gasströmung (DE-588)4156052-8 gnd rswk-swf Interstellares Gas (DE-588)4162147-5 gnd rswk-swf 1\p (DE-588)1071861417 Konferenzschrift 1987 Cambridge gnd-content Interstellares Gas (DE-588)4162147-5 s Gasströmung (DE-588)4156052-8 s 2\p DE-604 https://doi.org/10.1007/978-94-009-2953-1 Verlag Volltext 1\p cgwrk 20201028 DE-101 https://d-nb.info/provenance/plan#cgwrk 2\p cgwrk 20201028 DE-101 https://d-nb.info/provenance/plan#cgwrk |
| spellingShingle | Fabian, A. C. Cooling Flows in Clusters and Galaxies Physics Astronomy, Observations and Techniques Gasströmung (DE-588)4156052-8 gnd Interstellares Gas (DE-588)4162147-5 gnd |
| subject_GND | (DE-588)4156052-8 (DE-588)4162147-5 (DE-588)1071861417 |
| title | Cooling Flows in Clusters and Galaxies |
| title_alt | Proceedings of the NATO Advanced Research Workshop, Cambridge, U.K., June 22-26, 1987 |
| title_auth | Cooling Flows in Clusters and Galaxies |
| title_exact_search | Cooling Flows in Clusters and Galaxies |
| title_full | Cooling Flows in Clusters and Galaxies edited by A. C. Fabian |
| title_fullStr | Cooling Flows in Clusters and Galaxies edited by A. C. Fabian |
| title_full_unstemmed | Cooling Flows in Clusters and Galaxies edited by A. C. Fabian |
| title_short | Cooling Flows in Clusters and Galaxies |
| title_sort | cooling flows in clusters and galaxies |
| topic | Physics Astronomy, Observations and Techniques Gasströmung (DE-588)4156052-8 gnd Interstellares Gas (DE-588)4162147-5 gnd |
| topic_facet | Physics Astronomy, Observations and Techniques Gasströmung Interstellares Gas Konferenzschrift 1987 Cambridge |
| url | https://doi.org/10.1007/978-94-009-2953-1 |
| work_keys_str_mv | AT fabianac coolingflowsinclustersandgalaxies AT fabianac proceedingsofthenatoadvancedresearchworkshopcambridgeukjune22261987 |