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암흑 에너지 (Korean Wikipedia)

Analysis of information sources in references of the Wikipedia article "암흑 에너지" in Korean language version.

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51arxiv.org
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  • Peebles, P. J. E.; Ratra, Bharat (2003). "The cosmological constant and dark energy". Reviews of Modern Physics. 75 (2): 559–606. arXiv:astro-ph/0207347.
  • Idicherian Lonappan, Anto; Kumar, Sumit; R, Ruchika; Ananda Sen, Anjan (21 February 2018). "Bayesian evidences for dark energy models in light of current observational data". Physical Review D. 97 (4): 043524. arXiv:1707.00603.
  • Ade, P. A. R.; Aghanim, N.; Alves, M. I. R.; et al. (Planck Collaboration) (22 March 2013). "Planck 2013 results. I. Overview of products and scientific results – Table 9". Astronomy and Astrophysics. 571: A1. arXiv:1303.5062.
  • Paul J. Steinhardt; Neil Turok (2006). "Why the cosmological constant is small and positive". Science. 312 (5777): 1180–1183. arXiv:astro-ph/0605173.
  • Kragh, H (2012). "Preludes to dark energy: zero-point energy and vacuum speculations". Archive for History of Exact Sciences. 66 (3): 199–240. arXiv:1111.4623.
  • Buchert, T; Carfora, M; Ellis, G F R; Kolb, E W; MacCallum, M A H; Ostrowski, J J; Räsänen, S; Roukema, B F; Andersson, L; Coley, A A; Wiltshire, D L (5 November 2015). "Is there proof that backreaction of inhomogeneities is irrelevant in cosmology?". Classical and Quantum Gravity. 32 (21): 215021. arXiv:1505.07800.
  • [16] Clarkson, Chris; Ellis, George; Larena, Julien; Umeh, Obinna (1 November 2011). "Does the growth of structure affect our dynamical models of the Universe? The averaging, backreaction, and fitting problems in cosmology". Reports on Progress in Physics. 74 (11): 112901. arXiv:1109.2314.
  • Harvey, Alex (2012). "How Einstein Discovered Dark Energy". arXiv:1211.6338 physics.hist-ph).
  • Riess, Adam G.; Filippenko; Challis; Clocchiatti; Diercks; Garnavich; Gilliland; Hogan; Jha; Kirshner; Leibundgut; Phillips; Reiss; Schmidt; Schommer; Smith; Spyromilio; Stubbs; Suntzeff; Tonry (1998). "Observational evidence from supernovae for an accelerating universe and a cosmological constant". Astronomical Journal. 116 (3): 1009–1038. arXiv:astro-ph/9805201.
  • Perlmutter, S.; Aldering; Goldhaber; Knop; Nugent; Castro; Deustua; Fabbro; Goobar; Groom; Hook; Kim; Kim; Lee; Nunes; Pain; Pennypacker; Quimby; Lidman; Ellis; Irwin; McMahon; Ruiz-Lapuente; Walton; Schaefer; Boyle; Filippenko; Matheson; Fruchter; et al. (1999). "Measurements of Omega and Lambda from 42 high redshift supernovae". '"Astrophysical Journal. 517 (2): 565–586. arXiv:astro-ph/9812133.
  • The first appearance of the term "dark energy" is in the article with another cosmologist and Turner's student at the time, Dragan Huterer, "Prospects for Probing the Dark Energy via Supernova Distance Measurements", which was posted to the ArXiv.org e-print archive in August 1998 and published in Huterer, D.; Turner, M. (1999). "Prospects for probing the dark energy via supernova distance measurements". Physical Review D. 60 (8): 081301. arXiv:astro-ph/9808133., although the manner in which the term is treated there suggests it was already in general use. Cosmologist Saul Perlmutter has credited Turner with coining the term in an article Archived 2006년 8월 11일 - 웨이백 머신 they wrote together with Martin White, where it is introduced in quotation marks as if it were a neologism. Perlmutter, S.; Turner, M.; White, M. (1999). "Constraining Dark Energy with Type Ia Supernovae and Large-Scale Structure". Physical Review Letters. 83 (4): 670–673. arXiv:astro-ph/9901052.
  • Astier, Pierre (Supernova Legacy Survey); Guy; Regnault; Pain; Aubourg; Balam; Basa; Carlberg; Fabbro; Fouchez; Hook; Howell; Lafoux; Neill; Palanque-Delabrouille; Perrett; Pritchet; Rich; Sullivan; Taillet; Aldering; Antilogus; Arsenijevic; Balland; Baumont; Bronder; Courtois; Ellis; Filiol; et al. (2006). "The Supernova legacy survey: Measurement of ΩM, ΩΛ and W from the first year data set". Astronomy and Astrophysics. 447 (1): 31–48. arXiv:astro-ph/0510447.
  • Durrer, R. (2011). "What do we really know about Dark Energy?". Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences. 369 (1957): 5102–5114. arXiv:1103.5331.
  • Durrer, R. (2011). "What do we really know about dark energy?". Philosophical Transactions of the Royal Society A. 369 (1957): 5102–5114. arXiv:1103.5331.
  • Kowalski, Marek; Rubin, David; Aldering, G.; Agostinho, R. J.; Amadon, A.; Amanullah, R.; Balland, C.; Barbary, K.; Blanc, G.; Challis, P. J.; Conley, A.; Connolly, N. V.; Covarrubias, R.; Dawson, K. S.; Deustua, S. E.; Ellis, R.; Fabbro, S.; Fadeyev, V.; Fan, X.; Farris, B.; Folatelli, G.; Frye, B. L.; Garavini, G.; Gates, E. L.; Germany, L.; Goldhaber, G.; Goldman, B.; Goobar, A.; Groom, D. E.; et al. (27 October 2008). "Improved Cosmological Constraints from New, Old and Combined Supernova Datasets". The Astrophysical Journal. 686 (2): 749–778. arXiv:0804.4142. They find a best-fit value of the dark energy density, ΩΛ of 0.713+0.027–0.029(stat)+0.036–0.039(sys), of the total matter density, ΩM, of 0.274+0.016–0.016(stat)+0.013–0.012(sys) with an equation of state parameter w of −0.969+0.059–0.063(stat)+0.063–0.066(sys).
  • Crittenden; Neil Turok (1996). "Looking for $\Lambda$ with the Rees-Sciama Effect". Physical Review Letters. 76 (4): 575–578. arXiv:astro-ph/9510072.
  • Shirley Ho; Hirata; Nikhil Padmanabhan; Uros Seljak; Neta Bahcall (2008). "Correlation of CMB with large-scale structure: I. ISW Tomography and Cosmological Implications". Physical Review D. 78 (4): 043519. arXiv:0801.0642.
  • Tommaso Giannantonio; Ryan Scranton; Crittenden; Nichol; Boughn; Myers; Richards (2008). "Combined analysis of the integrated Sachs–Wolfe effect and cosmological implications". Physical Review D. 77 (12): 123520. arXiv:0801.4380.
  • Zelong Yi; Tongjie Zhang (2007). "Constraints on holographic dark energy models using the differential ages of passively evolving galaxies". Modern Physics Letters A. 22 (1): 41–54. arXiv:astro-ph/0605596.
  • Haoyi Wan; Zelong Yi; Tongjie Zhang; Jie Zhou (2007). "Constraints on the DGP Universe Using Observational Hubble parameter". Physics Letters B. 651 (5): 1368–1379. arXiv:0706.2723.
  • Cong Ma; Tongjie Zhang (2011). "Power of observational Hubble parameter data: a figure of merit exploration". Astrophysical Journal. 730 (2): 74. arXiv:1007.3787.
  • Joan Simon; Licia Verde; Raul Jimenez (2005). "Constraints on the redshift dependence of the dark energy potential". Physical Review D. 71 (12): 123001. arXiv:astro-ph/0412269.
  • Carroll, Sean M. (1998). "Quintessence and the Rest of the World: Suppressing Long-Range Interactions". Physical Review Letters. 81 (15): 3067–3070. arXiv:astro-ph/9806099.
  • Steinhardt, Paul J.; Wang, Li-Min; Zlatev, Ivaylo (1999). "Cosmological tracking solutions". Phys. Rev. D59 (12): 123504. arXiv:astro-ph/9812313.
  • Cai, Yi-Fu; Saridakis, Emmanuel N.; Setare, Mohammed R.; Xia, Jun-Qing (22 April 2010). "Quintom Cosmology - theoretical implications and observations". Physics Reports. 493 (1): 1–60. arXiv:0909.2776.
  • R.R.Caldwell (2002). "A phantom menace? Cosmological consequences of a dark energy component with super-negative equation of state". Physics Letters B. 545 (1–2): 23–29. arXiv:astro-ph/9908168.
  • Krishnan, Chethan; Mohayaee, Roya; Colgáin, Eoin Ó; Sheikh-Jabbari, M. M.; Yin, Lu (16 September 2021). "Does Hubble Tension Signal a Breakdown in FLRW Cosmology?". Classical and Quantum Gravity. 38 (18): 184001. arXiv:2105.097.
  • Rafael J. F. Marcondes (5 October 2016). "Interacting dark energy models in Cosmology and large-scale structure observational tests". arXiv:1610.01272 astro-ph.CO.
  • Exirifard, Q. (2011). "Phenomenological covariant approach to gravity". General Relativity and Gravitation. 43 (1): 93–106. arXiv:0808.1962.
  • Vagnozzi, Sunny; Visinelli, Luca; Mena, Olga; Mota, David F. (2020). "Do we have any hope of detecting scattering between dark energy and baryons through cosmology?". Monthly Notices of the Royal Astronomical Society. 493 (1): 1139–1152. arXiv:1911.12374.
  • Sunny Vagnozzi; Luca Visinelli; Philippe Brax; Anne-Christine Davis; Jeremy Sakstein (2021). "Direct detection of dark energy: The XENON1T excess and future prospects". Physical Review D. 104 (6): 063023. arXiv:2103.15834.
  • Chevallier, M; Polarski, D (2001). "Accelerating Universes with Scaling Dark Matter". International Journal of Modern Physics D. 10 (2): 213–224. arXiv:gr-qc/0009008.
  • Linder, Eric V. (3 March 2003). "Exploring the Expansion History of the Universe". Physical Review Letters. 90 (9): 091301. arXiv:astro-ph/0208512.
  • Barboza, E.M.; Alcaniz, J.S. (2008). "A parametric model for dark energy". Physics Letters B. 666 (5): 415–419. arXiv:0805.1713.
  • Jassal, H.K; Bagla, J.S (2010). "Understanding the origin of CMB constraints on Dark Energy". Monthly Notices of the Royal Astronomical Society. 405 (4): 2639–2650. arXiv:astro-ph/0601389.
  • Wetterich, C. (2004). "Phenomenological parameterization of quintessence". Physics Letters B. 594 (1–2): 17–22. arXiv:astro-ph/0403289.
  • Wiltshire, David L. (2007). "Exact Solution to the Averaging Problem in Cosmology". Physical Review Letters. 99 (25): 251101. arXiv:0709.0732.
  • Ishak, Mustapha; Richardson, James; Garred, David; Whittington, Delilah; Nwankwo, Anthony; Sussman, Roberto (2008). "Dark Energy or Apparent Acceleration Due to a Relativistic Cosmological Model More Complex than FLRW?". Physical Review D. 78 (12): 123531. arXiv:0708.2943.
  • Mattsson, Teppo (2010). "Dark energy as a mirage". Gen. Rel. Grav. 42 (3): 567–599. arXiv:0711.4264.
  • Wiltshire, D. (2008). "Cosmological equivalence principle and the weak-field limit". Physical Review D. 78 (8): 084032. arXiv:0809.1183.
  • Tsagas, Christos G. (2011). "Peculiar motions, accelerated expansion, and the cosmological axis". Physical Review D. 84 (6): 063503. arXiv:1107.4045.
  • D. O. Sabulsky; I. Dutta; E. A. Hinds; B. Elder; C. Burrage; E. J. Copeland (2019). "Experiment to Detect Dark Energy Forces Using Atom Interferometry". Physical Review Letters. 123 (6): 061102. arXiv:1812.08244.
  • Rubin, D.; Heitlauf, J. (6 May 2020). "Is the Expansion of the Universe Accelerating? All Signs Still Point to Yes: A Local Dipole Anisotropy Cannot Explain Dark Energy". The Astrophysical Journal. 894 (1): 68. arXiv:1912.02191.
  • Kang, Yijung; et al. (2020). "Early-type Host Galaxies of Type Ia Supernovae. II. Evidence for Luminosity Evolution in Supernova Cosmology". The Astrophysical Journal. 889 (1): 8. arXiv:1912.04903.
  • See M. Sami; R. Myrzakulov (2015). "Late time cosmic acceleration: ABCD of dark energy and modified theories of gravity". International Journal of Modern Physics D. 25 (12): 1630031. arXiv:1309.4188.
  • Lombriser, Lucas; Lima, Nelson (2017). "Challenges to Self-Acceleration in Modified Gravity from Gravitational Waves and Large-Scale Structure". Physics Letters B. 765: 382–385. arXiv:1602.07670.
  • Frieman, Joshua A.; Turner, Michael S.; Huterer, Dragan (1 January 2008). "Dark Energy and the Accelerating Universe". Annual Review of Astronomy and Astrophysics. 46 (1): 385–432. arXiv:0803.0982.
  • Loeb, Abraham (2002). "The Long-Term Future of Extragalactic Astronomy". Physical Review D. 65 (4): 047301. arXiv:astro-ph/0107568.
  • Krauss, Lawrence M.; Robert J. Scherrer (2007). "The Return of a Static Universe and the End of Cosmology". General Relativity and Gravitation. 39 (10): 1545–1550. arXiv:0704.0221.
  • Steinhardt, P. J.; Turok, N. (25 April 2002). "A Cyclic Model of the Universe". Science. 296 (5572): 1436–1439. arXiv:hep-th/0111030.
  • Merritt, David (2017). "Cosmology and convention". Studies in History and Philosophy of Science Part B: Studies in History and Philosophy of Modern Physics. 57: 41–52. arXiv:1703.02389.

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cam.ac.uk

cornell.edu

curious.astro.cornell.edu

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doi.org

esa.int

forbes.com

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hyperphysics.phy-astr.gsu.edu

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ui.adsabs.harvard.edu

  • The first paper, using observed data, which claimed a positive Lambda term was Paál, G.; et al. (1992). "Inflation and compactification from galaxy redshifts?". Astrophysics and Space Science. 191 (1): 107–124. Bibcode:1992Ap&SS.191..107P.
  • Ratra, Bharat; Peebles, P.J.E. (1988). "Cosmological consequences of a rolling homogeneous scalar field". Phys. Rev. D37 (12): 3406–3427. Bibcode:1988PhRvD..37.3406R.
  • Oztas, A.; Dil, E.; Smith, M.L. (2018). "The varying cosmological constant: a new approximation to the Friedmann equations and universe model". Mon. Not. R. Astron. Soc. 476 (1): 451–458. Bibcode:2018MNRAS.476..451O.
  • Oztas, A. (2018). "The effects of a varying cosmological constant on the particle horizon". Mon. Not. R. Astron. Soc. 481 (2): 2228–2234. Bibcode:2018MNRAS.481.2228O.
  • Clifton, Timothy; Ferreira, Pedro (April 2009). "Does Dark Energy Really Exist?". Scientific American. 300 (4): 48–55. Bibcode:2009SciAm.300d..48C.
  • Helbig, Phillip (2020). "Sonne und Mond, or, the good, the bad, and the ugly: comments on the debate between MOND and LambdaCDM". The Observatory. 140: 225–247. Bibcode:2020Obs...140..225H.

kuleuven.be

lirias.kuleuven.be

lbl.gov

  • The first appearance of the term "dark energy" is in the article with another cosmologist and Turner's student at the time, Dragan Huterer, "Prospects for Probing the Dark Energy via Supernova Distance Measurements", which was posted to the ArXiv.org e-print archive in August 1998 and published in Huterer, D.; Turner, M. (1999). "Prospects for probing the dark energy via supernova distance measurements". Physical Review D. 60 (8): 081301. arXiv:astro-ph/9808133., although the manner in which the term is treated there suggests it was already in general use. Cosmologist Saul Perlmutter has credited Turner with coining the term in an article Archived 2006년 8월 11일 - 웨이백 머신 they wrote together with Martin White, where it is introduced in quotation marks as if it were a neologism. Perlmutter, S.; Turner, M.; White, M. (1999). "Constraining Dark Energy with Type Ia Supernovae and Large-Scale Structure". Physical Review Letters. 83 (4): 670–673. arXiv:astro-ph/9901052.

msn.com

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science.nasa.gov

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map.gsfc.nasa.gov

nationalgeographic.com

ngm.nationalgeographic.com

nbcnews.com

newscientist.com

nih.gov

ncbi.nlm.nih.gov

nobelprize.org

npr.org

  • Using Tiny Particles To Answer Giant Questions. Science Friday, 3 April 2009. 녹취록에 따르면 브라이언 그린은 말하기를 "사실 먼 미래에는 우리의 국부 은하와 은하계 영역을 제외하고 지금 우리가 보고 있는 모든 것이 사라질 것이다. 전 우주가 우리 눈앞에서 사라질 것이며, 실제로 우주론에 자금을 지원하는 것에 대한 나의 주장 중 하나이다. 우리는 기회가 있을 때 그것을 해야 한다."

nytimes.com

ox.ac.uk

phys.org

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einsteinpapers.press.princeton.edu

scientificamerican.com

space.com

swin.edu.au

wigglez.swin.edu.au

web.archive.org

wikipedia.org

en.wikipedia.org

  • Taken from Frieman, Turner, & Huterer (2008)[97](pp. 6, 44):
    "우주는 세 가지 뚜렷한 시대를 거쳤다:
    복사-지배 시대(Radiation-dominated era),   z ≳ 3000 ;
    물질-지배 시대(Matter-dominated era),   3000 ≳ z ≳ 0.5 ;
    암흑 에너지-지배 시대(Dark-energy-dominated era),   0.5 ≳ z .
    척도인자의 진화는 지배적인 에너지 형태에 의해 제어된다:
    ( w 는 상수).
    복사-지배 시대 동안에는,
    물질-지배 시대 동안에는,
    암흑 에너지-지배 시대에는,  w ≃ −1  로 가정하면, 점근적으로
    [97](p. 6)
    "종합하면 현재의 모든 데이터는 암흑 에너지의 존재에 대한 강력한 증거를 제공하는데; 암흑 에너지가 기여하는 임계 밀도의 비율을 제한하고, 0.76 ± 0.02 , 그리고 상태 방정식 매개변수는:
      w ≈ −1 ± 0.1 [stat.] ± 0.1 [sys.] ,
    w 는 상수로 가정한다. 이것은 우주가 적색편이  z ∼ 0.4 와 나이  t ∼ 10 Ga(십억년)에 가속하기 시작했음을 의미한다. 이러한 결과는 공고해서(robusf) - 제약 조건을 훼손하지 않고 한 가지 방법의 데이터를 제거할 수 있으며, 공간 평탄도의 가정을 포기해도 실질적으로 약화되지 않는다."[97](p. 44)