Corpo negro (Portuguese Wikipedia)

Analysis of information sources in references of the Wikipedia article "Corpo negro" in Portuguese language version.

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10google.com.br

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archive.org

Planck, M. (1914). The Theory of Heat Radiation. Masius, M. (transl.) (2nd ed.). P. Blakiston's Son & Co. OL 7154661M, pp. 9–10, §10

arxiv.org

Krishna Rajagopal; Frank Wilczek (2001). "6.2 Coling by Neutrino Emissions (pp. 2135-2136) – The Condensed Matter Physics of QCD". In Mikhail A. Shifman (ed.). At The Frontier of Particle Physics: Handbook of QCD (On the occasion of the 75th birthday of Professor Boris Ioffe). Vol. 3. Singapore: World Scientific. pp. 2061–2151. arXiv:hep-ph/0011333v2. CiteSeerX 10.1.1.344.2269. doi:10.1142/9789812810458_0043. ISBN 978-981-02-4969-4. S2CID 13606600. For the first 10^5–6 years of its life, the cooling of a neutron star is governed by the balance between heat capacity and the loss of heat by neutrino emission. ... Both the specific heat C_V and the neutrino emission rate L_ν are dominated by physics within T of the Fermi surface. ... The star will cool rapidly until its interior temperature is T < T_c ~ ∆, at which time the quark matter core will become inert and the further cooling history will be dominated by neutrino emission from the nuclear matter fraction of the star.

doi.org

dx.doi.org

Gama, Jose (6 de dezembro de 2014). «NISTunits: Fundamental Physical Constants and Unit Conversions from NIST». CRAN: Contributed Packages. Consultado em 18 de novembro de 2024

google.com.br

books.google.com.br

Mahmoud Massoud (2005). "§2.1 Blackbody radiation". Engineering thermofluids: thermodynamics, fluid mechanics, and heat transfer. Springer. p. 568. ISBN 978-3-540-22292-7.
The emissivity of a surface in principle depends upon frequency, angle of view, and temperature. However, by definition, the radiation from a gray body is simply proportional to that of a black body at the same temperature, so its emissivity does not depend upon frequency (or, equivalently, wavelength). See Massoud Kaviany (2002). "Figure 4.3(b): Behaviors of a gray (no wavelength dependence), diffuse (no directional dependence) and opaque (no transmission) surface". Principles of heat transfer. Wiley-IEEE. p. 381. ISBN 978-0-471-43463-4. and Ronald G. Driggers (2003). Encyclopedia of optical engineering, Volume 3. CRC Press. p. 2303. ISBN 978-0-8247-4252-2.
Kirchhoff, G. (1860c). "Ueber das Verhältniss zwischen dem Emissionsvermögen und dem Absorptionsvermögen der Körper für Wärme and Licht". Annalen der Physik und Chemie. 185 (2): 275–301. Bibcode:1860AnP...185..275K doi:10.1002/andp.18601850205 Translated by Guthrie, F. as Kirchhoff, G. (1860). "On the relation between the radiating and absorbing powers of different bodies for light and heat". Philosophical Magazine. Series 4. 20: 1–21.
Valeri P. Frolov; Andrei Zelnikov (2011). "Equation 9.7.1". Introduction to Black Hole Physics. Oxford University Press. p. 321. ISBN 978-0-19-969229-3.
Robert M Wald (2005). "The thermodynamics of black holes (pp. 1–38)". In Andrés Gomberoff; Donald Marolf (eds.). Lectures on Quantum Gravity. Springer Science & Business Media. p. 28. ISBN 978-0-387-23995-8. ... no results on black hole thermodynamics have been subject to any experimental or observational tests ...
A simple example is provided by Srivastava M. K. (2011). "Cooling by radiation". The Person Guide to Objective Physics for the IIT-JEE. Pearson Education India. p. 610. ISBN 978-81-317-5513-6.
M Vollmer; K-P Mõllmann (2011). "Figure 1.38: Some examples for temperature dependence of emissivity for different materials". Infrared Thermal Imaging: Fundamentals, Research and Applications. John Wiley & Sons. p. 45. ISBN 978-3-527-63087-5.
Robert Osiander; M. Ann Garrison Darrin; John Champion (2006). MEMS and Microstructures in aerospace applications. CRC Press. p. 187. ISBN 978-0-8247-2637-9.
Walter Lewin; Warren Goldstein (2011). "X-ray bursters!". For the love of physics. Simon and Schuster. pp. 251 ff. ISBN 978-1-4391-0827-7.
TE Strohmayer (2006). "Neutron star structure and fundamental physics". In John W. Mason (ed.). Astrophysics update, Volume 2. Birkhäuser. p. 41. ISBN 978-3-540-30312-1.

harvard.edu

ui.adsabs.harvard.edu

Kirchhoff, G. (1860c). "Ueber das Verhältniss zwischen dem Emissionsvermögen und dem Absorptionsvermögen der Körper für Wärme and Licht". Annalen der Physik und Chemie. 185 (2): 275–301. Bibcode:1860AnP...185..275K doi:10.1002/andp.18601850205 Translated by Guthrie, F. as Kirchhoff, G. (1860). "On the relation between the radiating and absorbing powers of different bodies for light and heat". Philosophical Magazine. Series 4. 20: 1–21.

hgh-infrared.com

Some authors describe sources of infrared radiation with emissivity greater than approximately 0.99 as a black body. See "What is a Blackbody and Infrared Radiation?" Education/Reference tab. Electro Optical Industries, Inc. 2008. Archived from the original on 7 March 2016. Retrieved 11 november 2024.

kde.org

docs.kde.org

«Radiação dos Corpos Negros». Consultado em 25 de novembro de 2012

nature.com

Chun, Ai Lin (2008). "Blacker than black". Nature Nanotechnology. doi:10.1038/nnano.2008.29

openlibrary.org

Planck, M. (1914). The Theory of Heat Radiation. Masius, M. (transl.) (2nd ed.). P. Blakiston's Son & Co. OL 7154661M, pp. 9–10, §10

psu.edu

citeseerx.ist.psu.edu

Krishna Rajagopal; Frank Wilczek (2001). "6.2 Coling by Neutrino Emissions (pp. 2135-2136) – The Condensed Matter Physics of QCD". In Mikhail A. Shifman (ed.). At The Frontier of Particle Physics: Handbook of QCD (On the occasion of the 75th birthday of Professor Boris Ioffe). Vol. 3. Singapore: World Scientific. pp. 2061–2151. arXiv:hep-ph/0011333v2. CiteSeerX 10.1.1.344.2269. doi:10.1142/9789812810458_0043. ISBN 978-981-02-4969-4. S2CID 13606600. For the first 10^5–6 years of its life, the cooling of a neutron star is governed by the balance between heat capacity and the loss of heat by neutrino emission. ... Both the specific heat C_V and the neutrino emission rate L_ν are dominated by physics within T of the Fermi surface. ... The star will cool rapidly until its interior temperature is T < T_c ~ ∆, at which time the quark matter core will become inert and the further cooling history will be dominated by neutrino emission from the nuclear matter fraction of the star.

sciencemadesimple.com

«Why is the Sky Blue?». Science Made Simple

semanticscholar.org

Krishna Rajagopal; Frank Wilczek (2001). "6.2 Coling by Neutrino Emissions (pp. 2135-2136) – The Condensed Matter Physics of QCD". In Mikhail A. Shifman (ed.). At The Frontier of Particle Physics: Handbook of QCD (On the occasion of the 75th birthday of Professor Boris Ioffe). Vol. 3. Singapore: World Scientific. pp. 2061–2151. arXiv:hep-ph/0011333v2. CiteSeerX 10.1.1.344.2269. doi:10.1142/9789812810458_0043. ISBN 978-981-02-4969-4. S2CID 13606600. For the first 10^5–6 years of its life, the cooling of a neutron star is governed by the balance between heat capacity and the loss of heat by neutrino emission. ... Both the specific heat C_V and the neutrino emission rate L_ν are dominated by physics within T of the Fermi surface. ... The star will cool rapidly until its interior temperature is T < T_c ~ ∆, at which time the quark matter core will become inert and the further cooling history will be dominated by neutrino emission from the nuclear matter fraction of the star.

ufpr.br

fisica.ufpr.br

Física UFPR. Acessada em 04 de dezembro de 2012.

web.archive.org

Some authors describe sources of infrared radiation with emissivity greater than approximately 0.99 as a black body. See "What is a Blackbody and Infrared Radiation?" Education/Reference tab. Electro Optical Industries, Inc. 2008. Archived from the original on 7 March 2016. Retrieved 11 november 2024.

wikipedia.org

pt.wikipedia.org

Figure modeled after E. Böhm-Vitense (1989). "Figure 4.9". Introduction to Stellar Astrophysics: Basic stellar observations and data. Cambridge University Press. p. 26. ISBN 978-0-521-34869-0.

en.wikipedia.org

Krishna Rajagopal; Frank Wilczek (2001). "6.2 Coling by Neutrino Emissions (pp. 2135-2136) – The Condensed Matter Physics of QCD". In Mikhail A. Shifman (ed.). At The Frontier of Particle Physics: Handbook of QCD (On the occasion of the 75th birthday of Professor Boris Ioffe). Vol. 3. Singapore: World Scientific. pp. 2061–2151. arXiv:hep-ph/0011333v2. CiteSeerX 10.1.1.344.2269. doi:10.1142/9789812810458_0043. ISBN 978-981-02-4969-4. S2CID 13606600. For the first 10^5–6 years of its life, the cooling of a neutron star is governed by the balance between heat capacity and the loss of heat by neutrino emission. ... Both the specific heat C_V and the neutrino emission rate L_ν are dominated by physics within T of the Fermi surface. ... The star will cool rapidly until its interior temperature is T < T_c ~ ∆, at which time the quark matter core will become inert and the further cooling history will be dominated by neutrino emission from the nuclear matter fraction of the star.

wiley.com

onlinelibrary.wiley.com

Kirchhoff, G. (1860c). "Ueber das Verhältniss zwischen dem Emissionsvermögen und dem Absorptionsvermögen der Körper für Wärme and Licht". Annalen der Physik und Chemie. 185 (2): 275–301. Bibcode:1860AnP...185..275K doi:10.1002/andp.18601850205 Translated by Guthrie, F. as Kirchhoff, G. (1860). "On the relation between the radiating and absorbing powers of different bodies for light and heat". Philosophical Magazine. Series 4. 20: 1–21.

worldscientific.com

Krishna Rajagopal; Frank Wilczek (2001). "6.2 Coling by Neutrino Emissions (pp. 2135-2136) – The Condensed Matter Physics of QCD". In Mikhail A. Shifman (ed.). At The Frontier of Particle Physics: Handbook of QCD (On the occasion of the 75th birthday of Professor Boris Ioffe). Vol. 3. Singapore: World Scientific. pp. 2061–2151. arXiv:hep-ph/0011333v2. CiteSeerX 10.1.1.344.2269. doi:10.1142/9789812810458_0043. ISBN 978-981-02-4969-4. S2CID 13606600. For the first 10^5–6 years of its life, the cooling of a neutron star is governed by the balance between heat capacity and the loss of heat by neutrino emission. ... Both the specific heat C_V and the neutrino emission rate L_ν are dominated by physics within T of the Fermi surface. ... The star will cool rapidly until its interior temperature is T < T_c ~ ∆, at which time the quark matter core will become inert and the further cooling history will be dominated by neutrino emission from the nuclear matter fraction of the star.