Gauge Theory and the Early Universe:
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
248 |
| Schlagworte: | |
| Online-Zugang: | Volltext |
| Beschreibung: | P. de Bernardis, S. Masi , G. Moreno Dipartimento di Fisica, Universita' "La Sapienza" 00184 Roma Italy ABSTRACT. Anisotropy measurement techniques and results are reviewed, with special attention given to experimental problems. The cosmological relevance of the dipole anisotropy, the only anisotropy truly detected in the Cosmic Background Radiation, is discussed. 1. INTRODUCTION Anisotropy of the Cosmic Background Radiation at 2.7 K (CBR hereafter) is a cosmological topic with a wide range of applications. In order to define anisotropy let us consider fig. 1 a, where the celestial sphere is shown with two beams A and B, with beamwidth 0 and angular separation e. We define the anisotropy of CBR at angular scale e in terms of the difference i'2,1 between the CBR flux I(ex,u) measured in the two beams. At small angular scales (e<I°) a "stochastic" approach is preferred, and the anisotropy is defined as .cJ I = £ (1) I e where the brackets indicate averages over the whole celestial sphere. At large angular scales e>l° a deterministic approach is preferred, and the CBR flux I(ex, S) is expressed as a sum of spherical harmonics (2) I (ex, S) = I ~ aIm Y (ex, S) lm I,m The alm coefficients give the dipole, quadrupole and higher order components of the anisotropy. 257 P. Galeotti and D. N. Schramm (eds.), Gauge Theory and the Early Universe, 257-282 |
| Beschreibung: | 1 Online-Ressource (388p) |
| ISBN: | 9789400930599 9789401078764 |
| ISSN: | 1389-2185 |
| DOI: | 10.1007/978-94-009-3059-9 |
Internformat
MARC
| LEADER | 00000nmm a2200000zcb4500 | ||
|---|---|---|---|
| 001 | BV042415086 | ||
| 003 | DE-604 | ||
| 005 | 00000000000000.0 | ||
| 007 | cr|uuu---uuuuu | ||
| 008 | 150316s1988 |||| o||u| ||||||eng d | ||
| 020 | |a 9789400930599 |c Online |9 978-94-009-3059-9 | ||
| 020 | |a 9789401078764 |c Print |9 978-94-010-7876-4 | ||
| 024 | 7 | |a 10.1007/978-94-009-3059-9 |2 doi | |
| 035 | |a (OCoLC)863790230 | ||
| 035 | |a (DE-599)BVBBV042415086 | ||
| 040 | |a DE-604 |b ger |e aacr | ||
| 041 | 0 | |a eng | |
| 049 | |a DE-91 |a DE-83 | ||
| 082 | 0 | |a 523.01 |2 23 | |
| 084 | |a PHY 000 |2 stub | ||
| 100 | 1 | |a Galeotti, P. |e Verfasser |4 aut | |
| 245 | 1 | 0 | |a Gauge Theory and the Early Universe |c edited by P. Galeotti, David N. Schramm |
| 246 | 1 | 3 | |a Proceedings of the NATO Advanced Study Institute, Erice, Italy, May 20-30, 1986 |
| 264 | 1 | |a Dordrecht |b Springer Netherlands |c 1988 | |
| 300 | |a 1 Online-Ressource (388p) | ||
| 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 248 |x 1389-2185 | |
| 500 | |a P. de Bernardis, S. Masi , G. Moreno Dipartimento di Fisica, Universita' "La Sapienza" 00184 Roma Italy ABSTRACT. Anisotropy measurement techniques and results are reviewed, with special attention given to experimental problems. The cosmological relevance of the dipole anisotropy, the only anisotropy truly detected in the Cosmic Background Radiation, is discussed. 1. INTRODUCTION Anisotropy of the Cosmic Background Radiation at 2.7 K (CBR hereafter) is a cosmological topic with a wide range of applications. In order to define anisotropy let us consider fig. 1 a, where the celestial sphere is shown with two beams A and B, with beamwidth 0 and angular separation e. We define the anisotropy of CBR at angular scale e in terms of the difference i'2,1 between the CBR flux I(ex,u) measured in the two beams. At small angular scales (e<I°) a "stochastic" approach is preferred, and the anisotropy is defined as .cJ I = £ (1) I e where the brackets indicate averages over the whole celestial sphere. At large angular scales e>l° a deterministic approach is preferred, and the CBR flux I(ex, S) is expressed as a sum of spherical harmonics (2) I (ex, S) = I ~ aIm Y (ex, S) lm I,m The alm coefficients give the dipole, quadrupole and higher order components of the anisotropy. 257 P. Galeotti and D. N. Schramm (eds.), Gauge Theory and the Early Universe, 257-282 | ||
| 650 | 4 | |a Physics | |
| 650 | 4 | |a Nuclear physics | |
| 650 | 4 | |a Astrophysics and Astroparticles | |
| 650 | 4 | |a Classical and Quantum Gravitation, Relativity Theory | |
| 650 | 4 | |a Nuclear Physics, Heavy Ions, Hadrons | |
| 700 | 1 | |a Schramm, David N. |e Sonstige |4 oth | |
| 856 | 4 | 0 | |u https://doi.org/10.1007/978-94-009-3059-9 |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:BVB01-027850579 | ||
Datensatz im Suchindex
| _version_ | 1804153081706840064 |
|---|---|
| any_adam_object | |
| author | Galeotti, P. |
| author_facet | Galeotti, P. |
| author_role | aut |
| author_sort | Galeotti, P. |
| author_variant | p g pg |
| building | Verbundindex |
| bvnumber | BV042415086 |
| classification_tum | PHY 000 |
| collection | ZDB-2-PHA ZDB-2-BAE |
| ctrlnum | (OCoLC)863790230 (DE-599)BVBBV042415086 |
| dewey-full | 523.01 |
| dewey-hundreds | 500 - Natural sciences and mathematics |
| dewey-ones | 523 - Specific celestial bodies and phenomena |
| dewey-raw | 523.01 |
| dewey-search | 523.01 |
| dewey-sort | 3523.01 |
| dewey-tens | 520 - Astronomy and allied sciences |
| discipline | Physik |
| doi_str_mv | 10.1007/978-94-009-3059-9 |
| format | Electronic eBook |
| fullrecord | <?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>02924nmm a2200445zcb4500</leader><controlfield tag="001">BV042415086</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">9789400930599</subfield><subfield code="c">Online</subfield><subfield code="9">978-94-009-3059-9</subfield></datafield><datafield tag="020" ind1=" " ind2=" "><subfield code="a">9789401078764</subfield><subfield code="c">Print</subfield><subfield code="9">978-94-010-7876-4</subfield></datafield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1007/978-94-009-3059-9</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(OCoLC)863790230</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-599)BVBBV042415086</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">523.01</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">Galeotti, P.</subfield><subfield code="e">Verfasser</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Gauge Theory and the Early Universe</subfield><subfield code="c">edited by P. Galeotti, David N. Schramm</subfield></datafield><datafield tag="246" ind1="1" ind2="3"><subfield code="a">Proceedings of the NATO Advanced Study Institute, Erice, Italy, May 20-30, 1986</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 (388p)</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">248</subfield><subfield code="x">1389-2185</subfield></datafield><datafield tag="500" ind1=" " ind2=" "><subfield code="a">P. de Bernardis, S. Masi , G. Moreno Dipartimento di Fisica, Universita' "La Sapienza" 00184 Roma Italy ABSTRACT. Anisotropy measurement techniques and results are reviewed, with special attention given to experimental problems. The cosmological relevance of the dipole anisotropy, the only anisotropy truly detected in the Cosmic Background Radiation, is discussed. 1. INTRODUCTION Anisotropy of the Cosmic Background Radiation at 2.7 K (CBR hereafter) is a cosmological topic with a wide range of applications. In order to define anisotropy let us consider fig. 1 a, where the celestial sphere is shown with two beams A and B, with beamwidth 0 and angular separation e. We define the anisotropy of CBR at angular scale e in terms of the difference i'2,1 between the CBR flux I(ex,u) measured in the two beams. At small angular scales (e<I°) a "stochastic" approach is preferred, and the anisotropy is defined as .cJ I = £ (1) I e where the brackets indicate averages over the whole celestial sphere. At large angular scales e>l° a deterministic approach is preferred, and the CBR flux I(ex, S) is expressed as a sum of spherical harmonics (2) I (ex, S) = I ~ aIm Y (ex, S) lm I,m The alm coefficients give the dipole, quadrupole and higher order components of the anisotropy. 257 P. Galeotti and D. N. Schramm (eds.), Gauge Theory and the Early Universe, 257-282</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Physics</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Nuclear physics</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Astrophysics and Astroparticles</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Classical and Quantum Gravitation, Relativity Theory</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Nuclear Physics, Heavy Ions, Hadrons</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Schramm, David N.</subfield><subfield code="e">Sonstige</subfield><subfield code="4">oth</subfield></datafield><datafield tag="856" ind1="4" ind2="0"><subfield code="u">https://doi.org/10.1007/978-94-009-3059-9</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:BVB01-027850579</subfield></datafield></record></collection> |
| id | DE-604.BV042415086 |
| illustrated | Not Illustrated |
| indexdate | 2024-07-10T01:20:56Z |
| institution | BVB |
| isbn | 9789400930599 9789401078764 |
| issn | 1389-2185 |
| language | English |
| oai_aleph_id | oai:aleph.bib-bvb.de:BVB01-027850579 |
| oclc_num | 863790230 |
| open_access_boolean | |
| owner | DE-91 DE-BY-TUM DE-83 |
| owner_facet | DE-91 DE-BY-TUM DE-83 |
| physical | 1 Online-Ressource (388p) |
| 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 | Galeotti, P. Verfasser aut Gauge Theory and the Early Universe edited by P. Galeotti, David N. Schramm Proceedings of the NATO Advanced Study Institute, Erice, Italy, May 20-30, 1986 Dordrecht Springer Netherlands 1988 1 Online-Ressource (388p) txt rdacontent c rdamedia cr rdacarrier NATO ASI Series, Series C: Mathematical and Physical Sciences 248 1389-2185 P. de Bernardis, S. Masi , G. Moreno Dipartimento di Fisica, Universita' "La Sapienza" 00184 Roma Italy ABSTRACT. Anisotropy measurement techniques and results are reviewed, with special attention given to experimental problems. The cosmological relevance of the dipole anisotropy, the only anisotropy truly detected in the Cosmic Background Radiation, is discussed. 1. INTRODUCTION Anisotropy of the Cosmic Background Radiation at 2.7 K (CBR hereafter) is a cosmological topic with a wide range of applications. In order to define anisotropy let us consider fig. 1 a, where the celestial sphere is shown with two beams A and B, with beamwidth 0 and angular separation e. We define the anisotropy of CBR at angular scale e in terms of the difference i'2,1 between the CBR flux I(ex,u) measured in the two beams. At small angular scales (e<I°) a "stochastic" approach is preferred, and the anisotropy is defined as .cJ I = £ (1) I e where the brackets indicate averages over the whole celestial sphere. At large angular scales e>l° a deterministic approach is preferred, and the CBR flux I(ex, S) is expressed as a sum of spherical harmonics (2) I (ex, S) = I ~ aIm Y (ex, S) lm I,m The alm coefficients give the dipole, quadrupole and higher order components of the anisotropy. 257 P. Galeotti and D. N. Schramm (eds.), Gauge Theory and the Early Universe, 257-282 Physics Nuclear physics Astrophysics and Astroparticles Classical and Quantum Gravitation, Relativity Theory Nuclear Physics, Heavy Ions, Hadrons Schramm, David N. Sonstige oth https://doi.org/10.1007/978-94-009-3059-9 Verlag Volltext |
| spellingShingle | Galeotti, P. Gauge Theory and the Early Universe Physics Nuclear physics Astrophysics and Astroparticles Classical and Quantum Gravitation, Relativity Theory Nuclear Physics, Heavy Ions, Hadrons |
| title | Gauge Theory and the Early Universe |
| title_alt | Proceedings of the NATO Advanced Study Institute, Erice, Italy, May 20-30, 1986 |
| title_auth | Gauge Theory and the Early Universe |
| title_exact_search | Gauge Theory and the Early Universe |
| title_full | Gauge Theory and the Early Universe edited by P. Galeotti, David N. Schramm |
| title_fullStr | Gauge Theory and the Early Universe edited by P. Galeotti, David N. Schramm |
| title_full_unstemmed | Gauge Theory and the Early Universe edited by P. Galeotti, David N. Schramm |
| title_short | Gauge Theory and the Early Universe |
| title_sort | gauge theory and the early universe |
| topic | Physics Nuclear physics Astrophysics and Astroparticles Classical and Quantum Gravitation, Relativity Theory Nuclear Physics, Heavy Ions, Hadrons |
| topic_facet | Physics Nuclear physics Astrophysics and Astroparticles Classical and Quantum Gravitation, Relativity Theory Nuclear Physics, Heavy Ions, Hadrons |
| url | https://doi.org/10.1007/978-94-009-3059-9 |
| work_keys_str_mv | AT galeottip gaugetheoryandtheearlyuniverse AT schrammdavidn gaugetheoryandtheearlyuniverse AT galeottip proceedingsofthenatoadvancedstudyinstituteericeitalymay20301986 AT schrammdavidn proceedingsofthenatoadvancedstudyinstituteericeitalymay20301986 |