Linde, A. (2002). Inflationary Theory versus Ekpyrotic/Cyclic Scenario. arΧiv:hep-th/0205259 28 Temmuz 2013 tarihinde Wayback Machine sitesinde arşivlendi..
fr.arxiv.org
Voir par exemple (İngilizce) Leo Stodolsky, Some neutrino events of the 21st century, in Neutrino astrophysics, comptes rendus du quatrième atelier SFB-375, château de Ringberg, Allemagne, 20-24 octobre 1997, page 178-181, astro-ph/9801320 Voir en ligne 16 Kasım 2016 tarihinde Wayback Machine sitesinde arşivlendi..
Raghunathan Srianand, Patrick Petitjean & Cédric Ledoux, The microwave background temperature at the redshift of 2.33771, Nature, 408, 931 (2000), astro-ph/0012222 Voir en ligne 18 Mart 2017 tarihinde Wayback Machine sitesinde arşivlendi..
After 300,000 years, nuclei began to capture electrons and form the first atoms. This cosmic microwave map reveals what the Universe was like after 380,000 years. The red and yellow areas are slightly warmer than the blue and green ones and are a sign that matter was clumping.http://www.infoplease.com/dk/science/encyclopedia/big-bang.html 12 Ağustos 2011 tarihinde Wayback Machine sitesinde arşivlendi.
(6) When the cosmic microwave background radiation was emitted during atom formation 300,000 years after the Big Bang, its temperature was several thousand degrees and the light was in the visible part of the electromagnetic spectrum. As the Universe expanded, it cooled and the visible light first became infrared radiation then microwaves. The temperature of the Universe now is a frigid 2.725 degrees about absolute zero.
(7) During the period in which atoms were forming and earlier, the Universe was opaque in the sense that light could not travel any appreciable distance. It was as though the Universe was "in a fog." At 380,000 years, recombination was essentially completed: Each proton had paired up with an electron to form a hydrogen atom. Light was liberated. The Universe cleared and the cosmic background radiation has traveled undisturbed ever since. When WMAP makes its measurements, it captures some of the radiation that has been traveling uninterrupted for almost 14 billion years.
http://www.jupiterscientific.org/sciinfo/ncupdate.html 1 Aralık 2008 tarihinde Wayback Machine sitesinde arşivlendi.
After most leptons and anti-leptons are annihilated at the end of the lepton epoch the energy of the universe is dominated by photons. These photons are still interacting frequently with charged protons, electrons and (eventually) nuclei, and continue to do so for the next 300,000 years.
http://www.wikinfo.org/index.php/Timeline_of_the_Universe 22 Kasım 2008 tarihinde Wayback Machine sitesinde arşivlendi.
http://map.gsfc.nasa.gov/media/080998/index.html 12 Ocak 2012 tarihinde Wayback Machine sitesinde arşivlendi.
After 300,000 years, nuclei began to capture electrons and form the first atoms. This cosmic microwave map reveals what the Universe was like after 380,000 years. The red and yellow areas are slightly warmer than the blue and green ones and are a sign that matter was clumping.http://www.infoplease.com/dk/science/encyclopedia/big-bang.html 12 Ağustos 2011 tarihinde Wayback Machine sitesinde arşivlendi.
(6) When the cosmic microwave background radiation was emitted during atom formation 300,000 years after the Big Bang, its temperature was several thousand degrees and the light was in the visible part of the electromagnetic spectrum. As the Universe expanded, it cooled and the visible light first became infrared radiation then microwaves. The temperature of the Universe now is a frigid 2.725 degrees about absolute zero.
(7) During the period in which atoms were forming and earlier, the Universe was opaque in the sense that light could not travel any appreciable distance. It was as though the Universe was "in a fog." At 380,000 years, recombination was essentially completed: Each proton had paired up with an electron to form a hydrogen atom. Light was liberated. The Universe cleared and the cosmic background radiation has traveled undisturbed ever since. When WMAP makes its measurements, it captures some of the radiation that has been traveling uninterrupted for almost 14 billion years.
http://www.jupiterscientific.org/sciinfo/ncupdate.html 1 Aralık 2008 tarihinde Wayback Machine sitesinde arşivlendi.
After most leptons and anti-leptons are annihilated at the end of the lepton epoch the energy of the universe is dominated by photons. These photons are still interacting frequently with charged protons, electrons and (eventually) nuclei, and continue to do so for the next 300,000 years.
http://www.wikinfo.org/index.php/Timeline_of_the_Universe 22 Kasım 2008 tarihinde Wayback Machine sitesinde arşivlendi.
http://map.gsfc.nasa.gov/media/080998/index.html 12 Ocak 2012 tarihinde Wayback Machine sitesinde arşivlendi.
After 300,000 years, nuclei began to capture electrons and form the first atoms. This cosmic microwave map reveals what the Universe was like after 380,000 years. The red and yellow areas are slightly warmer than the blue and green ones and are a sign that matter was clumping.http://www.infoplease.com/dk/science/encyclopedia/big-bang.html 12 Ağustos 2011 tarihinde Wayback Machine sitesinde arşivlendi.
(6) When the cosmic microwave background radiation was emitted during atom formation 300,000 years after the Big Bang, its temperature was several thousand degrees and the light was in the visible part of the electromagnetic spectrum. As the Universe expanded, it cooled and the visible light first became infrared radiation then microwaves. The temperature of the Universe now is a frigid 2.725 degrees about absolute zero.
(7) During the period in which atoms were forming and earlier, the Universe was opaque in the sense that light could not travel any appreciable distance. It was as though the Universe was "in a fog." At 380,000 years, recombination was essentially completed: Each proton had paired up with an electron to form a hydrogen atom. Light was liberated. The Universe cleared and the cosmic background radiation has traveled undisturbed ever since. When WMAP makes its measurements, it captures some of the radiation that has been traveling uninterrupted for almost 14 billion years.
http://www.jupiterscientific.org/sciinfo/ncupdate.html 1 Aralık 2008 tarihinde Wayback Machine sitesinde arşivlendi.
After most leptons and anti-leptons are annihilated at the end of the lepton epoch the energy of the universe is dominated by photons. These photons are still interacting frequently with charged protons, electrons and (eventually) nuclei, and continue to do so for the next 300,000 years.
http://www.wikinfo.org/index.php/Timeline_of_the_Universe 22 Kasım 2008 tarihinde Wayback Machine sitesinde arşivlendi.
http://map.gsfc.nasa.gov/media/080998/index.html 12 Ocak 2012 tarihinde Wayback Machine sitesinde arşivlendi.
Lemaître, G. (1931). "The Evolution of the Universe: Discussion". Nature 128: 699–701. doi: 10.1038/128704a0 25 Nisan 2009 tarihinde Wayback Machine sitesinde arşivlendi..
Raghunathan Srianand, Patrick Petitjean & Cédric Ledoux, The microwave background temperature at the redshift of 2.33771, Nature, 408, 931 (2000), astro-ph/0012222 Voir en ligne 18 Mart 2017 tarihinde Wayback Machine sitesinde arşivlendi..
After 300,000 years, nuclei began to capture electrons and form the first atoms. This cosmic microwave map reveals what the Universe was like after 380,000 years. The red and yellow areas are slightly warmer than the blue and green ones and are a sign that matter was clumping.http://www.infoplease.com/dk/science/encyclopedia/big-bang.html 12 Ağustos 2011 tarihinde Wayback Machine sitesinde arşivlendi.
(6) When the cosmic microwave background radiation was emitted during atom formation 300,000 years after the Big Bang, its temperature was several thousand degrees and the light was in the visible part of the electromagnetic spectrum. As the Universe expanded, it cooled and the visible light first became infrared radiation then microwaves. The temperature of the Universe now is a frigid 2.725 degrees about absolute zero.
(7) During the period in which atoms were forming and earlier, the Universe was opaque in the sense that light could not travel any appreciable distance. It was as though the Universe was "in a fog." At 380,000 years, recombination was essentially completed: Each proton had paired up with an electron to form a hydrogen atom. Light was liberated. The Universe cleared and the cosmic background radiation has traveled undisturbed ever since. When WMAP makes its measurements, it captures some of the radiation that has been traveling uninterrupted for almost 14 billion years.
http://www.jupiterscientific.org/sciinfo/ncupdate.html 1 Aralık 2008 tarihinde Wayback Machine sitesinde arşivlendi.
After most leptons and anti-leptons are annihilated at the end of the lepton epoch the energy of the universe is dominated by photons. These photons are still interacting frequently with charged protons, electrons and (eventually) nuclei, and continue to do so for the next 300,000 years.
http://www.wikinfo.org/index.php/Timeline_of_the_Universe 22 Kasım 2008 tarihinde Wayback Machine sitesinde arşivlendi.
http://map.gsfc.nasa.gov/media/080998/index.html 12 Ocak 2012 tarihinde Wayback Machine sitesinde arşivlendi.
Voir par exemple (İngilizce) Leo Stodolsky, Some neutrino events of the 21st century, in Neutrino astrophysics, comptes rendus du quatrième atelier SFB-375, château de Ringberg, Allemagne, 20-24 octobre 1997, page 178-181, astro-ph/9801320 Voir en ligne 16 Kasım 2016 tarihinde Wayback Machine sitesinde arşivlendi..
"Anisotropy". 7 Ocak 2009 tarihinde kaynağından arşivlendi. Erişim tarihi: 1 Şubat 2009.
Lemaître, G. (1931). "The Evolution of the Universe: Discussion". Nature 128: 699–701. doi: 10.1038/128704a0 25 Nisan 2009 tarihinde Wayback Machine sitesinde arşivlendi..
"Braneworld". 10 Haziran 2011 tarihinde kaynağından arşivlendi. Erişim tarihi: 1 Şubat 2009.
"Brane". 28 Temmuz 2009 tarihinde kaynağından arşivlendi. Erişim tarihi: 1 Şubat 2009.
"Ekpyrotic". 22 Ağustos 2009 tarihinde kaynağından arşivlendi. Erişim tarihi: 1 Şubat 2009.
Linde, A. (2002). Inflationary Theory versus Ekpyrotic/Cyclic Scenario. arΧiv:hep-th/0205259 28 Temmuz 2013 tarihinde Wayback Machine sitesinde arşivlendi..
After 300,000 years, nuclei began to capture electrons and form the first atoms. This cosmic microwave map reveals what the Universe was like after 380,000 years. The red and yellow areas are slightly warmer than the blue and green ones and are a sign that matter was clumping.http://www.infoplease.com/dk/science/encyclopedia/big-bang.html 12 Ağustos 2011 tarihinde Wayback Machine sitesinde arşivlendi.
(6) When the cosmic microwave background radiation was emitted during atom formation 300,000 years after the Big Bang, its temperature was several thousand degrees and the light was in the visible part of the electromagnetic spectrum. As the Universe expanded, it cooled and the visible light first became infrared radiation then microwaves. The temperature of the Universe now is a frigid 2.725 degrees about absolute zero.
(7) During the period in which atoms were forming and earlier, the Universe was opaque in the sense that light could not travel any appreciable distance. It was as though the Universe was "in a fog." At 380,000 years, recombination was essentially completed: Each proton had paired up with an electron to form a hydrogen atom. Light was liberated. The Universe cleared and the cosmic background radiation has traveled undisturbed ever since. When WMAP makes its measurements, it captures some of the radiation that has been traveling uninterrupted for almost 14 billion years.
http://www.jupiterscientific.org/sciinfo/ncupdate.html 1 Aralık 2008 tarihinde Wayback Machine sitesinde arşivlendi.
After most leptons and anti-leptons are annihilated at the end of the lepton epoch the energy of the universe is dominated by photons. These photons are still interacting frequently with charged protons, electrons and (eventually) nuclei, and continue to do so for the next 300,000 years.
http://www.wikinfo.org/index.php/Timeline_of_the_Universe 22 Kasım 2008 tarihinde Wayback Machine sitesinde arşivlendi.
http://map.gsfc.nasa.gov/media/080998/index.html 12 Ocak 2012 tarihinde Wayback Machine sitesinde arşivlendi.
Penrose, R. (1979). "Singularities and Time-Asymmetry". Hawking, S.W. (ed); Israel, W. (ed) General Relativity: An Einstein Centenary Survey: 581–638, Cambridge University Press.
Penrose, R. (1989). "Difficulties with Inflationary Cosmology". Fergus, E.J. (ed) Proceedings of the 14th Texas Symposium on Relativistic Astrophysics: 249-264, New York Academy of Sciences. doi: 10.1111/j.1749-6632.1989.tb50513.x.[ölü/kırık bağlantı], 2[ölü/kırık bağlantı]
