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£². Quantum nucleation of topological defects during inflation
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£µ. R.Basu, A.H.Guth, and A.Vilenkin, Phys. Rev. D44, 340(1991).
£±¡¥»á̾¡¤½ê°¡¤³Øǯ¡¿Àî¼ ¹ä¡Ê¤«¤ï¤à¤é ¤´¤¦¡Ë
¿·³ãÂç³Ø±§ÃèʪÍý³Ø¸¦µæ¼¼ £Í£²
£²¡¥È¯É½¥¿¥¤¥È¥ë¡¿For Obtaining Interior Solutions of the Kerr Metric
£³¡¥È¯É½ÆâÍƤ˴ؤ¹¤ë¥¡¼¥ï¡¼¥É¡¿the Kerr metric,interior solution,
the Newman-Janis algorithm,
boundary conditions,a trial solution
£´¡¥È¯É½ÆâÍƤΥ¢¥Ö¥¹¥È¥é¥¯¥È¡¿
EinsteinÊýÄø¼°¤Ë¤è¤êÅ·ÂΤ¬·ÁÀ®¤¹¤ë½ÅÎϾì¤Î²ò¤ò¹Í¤¨¤ë¾å¤Ç¡¤Å·ÂÎÆâÉô¤Ç
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º£²ó¤Ï¡¤Drake,Turolla Åù¤ÎÏÀʸ¤«¤éKerrÆâÉô²ò¤òµá¤á¤ë²áÄø¤ò¾Ò²ð¤¹¤ë¡£
¡¦KerrÆâÉô²ò¤òµá¤á¤ë¾å¤Ç¤Îº¤Æñ¤ÊÅÀ¡¿¡¦ÀÅŪµåÂоβò¤«¤éÄê¾ï¼´Âоβò¤òµá
¤á¤ë¤¿¤á¤Îthe Newman-Janis algorithm¡¿¡¦boundary conditions ¡¿¡¦°µÎÏ¡¤
Ì©ÅÙ¤ËÂФ¹¤ë¡¤ÊªÍýŪ¸«ÃϤ«¤é¤Î¾ò·ï¡¿¡¦trial solution¤È¸¡¾ÚÅù¡¤¤Ë¤Ä¤¤¤Æ
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S.P.Drake and R.Turolla:gr-qc/9703084
D.McManus:Class.Quant.Grav.8 863 (1991)
W.Israel:Nuovo Cim.44B 1 (1966)
E.T.Newman and A.I.Janis:J.Math.Phys.6 915 (1965)
S.Chandrasekhar:The Mathematical Theory of Black Holes
(Oxford University Press ,Oxford,1983)
£±¡¤¶ÌÃÖ¡¡¹§»ê¡¤Áá°ðÅÄÂç³ØÍý¹©³ØÉôÁ°Åĸ¦µæ¼¼£Í£²
£²¡¤Non-Abelian Black Holes in Brans-Dicke theory
£³¡¤Non-Abelian Black Hole ¡¤ Brans-Dicke theory
¡¡¡¡Black Hole thermodynamics¡¤ catastrophe theory
£´¡¤°ìÈÌÁêÂÐÀÍýÏÀ¤Ç¤Ï¤³¤ì¤Þ¤Ç²¿¼ïÎफ¤ÎÈó²Ä´¹¾ì¤òȼ¤¦Black Hole ²ò¤¬¿ôÃÍ
Ū¤Ëµá¤á¤é¤ì¡¤¤½¤ÎÀ¼Á¤âÄ´¤Ù¤é¤ì¤Æ¤¤¿¡¥º£²ó¤Ï¥¹¥«¥é¡¼¡¦¥Æ¥ó¥½¥ëÍýÏÀ¤Î
°ì¤Ä¤Ç¤¢¤ëBrans-Dicke theory ¤Ë¤ª¤¤¤ÆƱÍͤËÈó²Ä´¹¾ì¤òȼ¤¦Black Hole
²ò¤ò¿ôÃÍŪ¤Ëµá¤á¡¤¤½¤ÎÀ¼Á¤òÄ´¤Ù¡¤°ìÈÌÁêÂÐÀÍýÏÀ¤Î¾ì¹ç¤È¤Î°ã¤¤¤òµÄÏÀ¤¹
¤ë¡¥Brans-Dicke theory ¤ÏBrans-Dicke ¥Ñ¥é¥á¡¼¥¿¡¼¤È¸Æ¤Ð¤ì¤ë¥Ñ¥é¥á¡¼
¥¿¡¼¤Ë¤è¤Ã¤ÆÆÃħ¤Å¤±¤é¤ì¤Æ¤ª¤ê¡¤¤³¤Î¥Ñ¥é¥á¡¼¥¿¡¼¤¬Ìµ¸ÂÂç¤Î¶Ë¸Â¤Ç¤Ï°ìÈÌ
ÁêÂÐÀÍýÏÀ¤Ëµ¢Ã夵¤ì¤ë¡¥´Ñ¬Ū¤Ë¤Ï¤³¤Î¥Ñ¥é¥á¡¼¥¿¡¼¤Ï£µ£°£°°Ê¾å¤È¤ÎÀ©¸Â¤¬
¤¢¤ë¤¬¡¤¤½¤Î¤è¤¦¤ÊÀ©¸Â¤Î¤â¤È¤Ç¤Ï²ò¤Î¿¶¤ëÉñ¤¤¤Ï¤Û¤È¤ó¤É°ìÈÌÁêÂÐÀÍýÏÀ
¤Î¾ì¹ç¤È¶èÊ̤¬¤Ä¤«¤Ê¤¤¤³¤È¤¬¤ï¤«¤Ã¤¿¡¥¤¿¤À¤·¡¤¤³¤Î¥Ñ¥é¥á¡¼¥¿¡¼¤¬¾®¤µ¤¤
Îΰè¤Ç¤Ï²ò¶ÊÀþ¤¬°ìÈÌÁêÂÐÀÍýÏÀ¤Î¾ì¹ç¤ÈÄêÀŪ¤Ë°Û¤Ê¤ê¡¤Black Hole Ç®ÎϳØ
¤È¤Î´ØÏ¢¤Ç¤³¤Î»ö¤òÀâÌÀ¤¹¤ë¡¥
£µ¡¤[1] C. Brans and R.H. Dicke, Phys. Rev. 124, p925
(1961).
[2] K. Maeda, T. Tachizawa, T. Torii and T. Maki,
Phys. Rev. Lett. 72, p450 (1994),
T. Torii, K. Maeda, and T. Tachizawa,
Phys. Rev. D 51, p1510 (1995),
T. Tachizawa, K. Maeda, and T. Torii,
Phys. Rev. D 51, p4054 (1995).
[3] R. M. Wald, Phys. Rev. D 48, p3427 (1993),
V. Iyer and R. M. Wald, Phys. Rev. D 50, p846
(1994),
V. Iyer and R. M. Wald, Phys. Rev. D 52,
p4430 (1995).
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Piotr T Chrusciel and Robert M Wald:
"On the topology of stationary black holes"
Class.Quantum Grav.11(1994)L147
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5.»²¹Íʸ¸¥¡§Adiabatic Geometrical Phase for Scalar Fields in a Curved
Spacetime Ali Mostafazadeh hep-th/9608051
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5.J.Libson,J.Masso,E.Seidel,W.-M.Suen and P.Walker,Phys.Rev.D 53,4335
(1996),P.Anninos,D.Bernstein,S.Brandt,J.Libson,J.Masso,E.Seidel,
L.Smarr and P.Walker,Phys.Rev.Lett 74,630(1995)
1.Âç¾¾¹¬À¸¡¢Åìµþ¹©¶ÈÂç³ØÂç³Ø±¡Íý¹©³Ø¸¦µæ²ÊºÙëÀи¶¸¦µæ¼¼M£±
2.Rotation of the plane of polarization and geometry
3.blackholes, polarization, relativity, X-rays sources
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5.Paul A.Connors, Tsvi Piran, and Richard F.Stark:The Astrophysical
Journal,235:224-244,1980
1. ÅÄÂå ´ð·Ä ¡¢µþÅÔÂç³Ø Å·Âγ˸¦µæ¼¼ M£±
2. ¥¿¥¤¥È¥ë¡§Ì©ÅÙÍɤ餮¤È½ÅÎÏÇȤˤè¤ë Inflation Potential ¤ÎºÆ¹½À®
3. ¥¡¼¥ï¡¼¥É¡§inflation , slow roll approximation , potential ,
density perturbation , tensor perturbation
4. Abstract:
¥¤¥ó¥Õ¥é¥È¥ó¤Î¥Ý¥Æ¥ó¥·¥ã¥ë¤È¡¢¥¤¥ó¥Õ¥ì¡¼¥·¥ç¥ó¤Ë¤è¤Ã¤ÆÀ¸À®¤µ¤ì¤ëÌ©ÅÙ
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¤Î½¸ÀѤ¬Í½ÁÛ¤µ¤ì¤ë¤¬¡¢¤³¤ì¤é¤Î¥Ç¡¼¥¿¤Ë¤è¤Ã¤Æ±§Ãè½é´ü¤ÎÌ©ÅÙÍɤ餮¤È½ÅÎÏ
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5. Reference: J.E.Lidsey et al., astro-ph/9508078
1.ÀÖÅçÃÒÀ¬ ̾¸Å²°Âç³ØÍý³ØÉôCG¸¦ô¸ M1
2.The visualization by comuter graphics in general relativity
3."visualization","headon collision","embedding to 3-dim Euclid
space","Misner solution"
4.Visualization by acomputer can connect recognition of a man with a
physical event concretely.Therefore I carries out embedding to
3-dimensional Euclid space of relativistic two-dimensional
surface,and expresses the object on computer.I am going to obtain an
example of a concrete image of a physical event through it.I hope to
treat "two blackholes collision for Misner solution" as a example.
5.Visualization in Curved Spacetiome.II.Visualization of Surfaces via Embedding
author :Hans-Peter Nollert and Heinz Herold
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£³¡¥Cosmology,structure formation,Zel'dovich approximation,Wavelet analysis
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¤¹¤ë¤³¤È¤¬½ÐÍè¤ë¡£¤È¤³¤í¤¬Fourier²òÀϤǤϡ¢¤æ¤é¤®¤Î¥¹¥Ú¥¯¥È¥ë¤Ë´Ø¤¹¤ë¾ðÊó¤ò
ÆÀ¤ëÂå¤ï¤ê¤Ë¡¢¤æ¤é¤®¤Î°ÌÃ֤ξðÊó¤ò¼º¤Ã¤Æ¤·¤Þ¤¦¡£Fujiwara,Soda(1996)¤Ï¡¢°ÌÃÖ
¤Î¾ðÊó¤ò´Þ¤à¤â¤Î¤È¤·¤Æ¡¢Wavelet¤òÍѤ¤¤¿²òÀϤò¹Ô¤Ã¤¿¡£Wavelet²òÀϤǤÏFourier
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£µ¡¥[1] Y.Fujiwara and J.Soda, Prog. Theor. Phys. 95 (1996) 1059
[2] L.Z.Fang and J.Pando, preprint, astro-ph/9701228
[3] Ya.B.Zeldovich, Astron. Astrophys. 5 (1970) 84
[4] P.Catelan, MNRAS 276 (1995) 115
etc.
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¡Ö¥Ï¥¤¥Ö¥ê¥Ã¥É¥¤¥ó¥Õ¥ì¡¼¥·¥ç¥ó½ô¡¹¡×
key word:hybrid inflation
¡¡¥¤¥ó¥Õ¥ì¡¼¥·¥ç¥ó±§Ãè¥â¥Ç¥ë¤Ç¡¢¥¤¥ó¥Õ¥ì¡¼¥·¥ç¥ó¤¬½ªÎ»¤¹¤ëÊýË¡¤ÏÂ礤¯
ʬ¤±¤Æslow roll¡¢°ì¼¡Áêž°Ü¡¢water fall¤Î£³¼ïÎब¤¢¤ë¡£water fall·¿¤Î
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¤ì¤ë¡£¤½¤Î¿¤¯¤Î¥â¥Ç¥ë¤Ç¤ÏÉÔ¼«Á³¤Ë¾®¤µ¤Êcoupling constant¤ò²¾Äꤷ¤Ê¤¯
¤Æ¤âºÑ¤ß¡¢¤Þ¤¿¡¢supersymmetry¤ò¹Íθ¤ËÆþ¤ì¤¿ºÝ¡¢¼«Á³¤Ê¥â¥Ç¥ë¤ò¹½ÃÛ¤·¤ä
¤¹¤¤¡£º£²ó¤ÏLinde¤Ë¤è¤Ã¤ÆÄ󾧤µ¤ì¤¿¥Ï¥¤¥Ö¥ê¥Ã¥É¥¤¥ó¥Õ¥ì¡¼¥·¥ç¥ó¤È¡¢¤½
¤Îº£¸å¤ÎŸ˾¤Ë¤Ä¤¤¤Æ¾Ò²ð¤¹¤ë¡£
refs.¡¦A.D.Linde,Phys.Lett.B,259,38(1991)
¡¦A.D.Linde,Phys.Rev.D,49,748,(1994) etc.
1. »á̾: ²¬Éô ¹§¹°¡Ê¤ª¤«¤Ù ¤¿¤«¤Ò¤í¡Ë
½ê°: ÅìµþÂç³ØÂç³Ø±¡Íý³Ø·Ï¸¦µæ²Ê ±§ÃèÍýÏÀ¸¦µæ¼¼
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2. ¥¿¥¤¥È¥ë :Cosmological gamma ray bursts and
the ultra high energy cosmic rays
3. ¥¡¼¥ï¡¼¥É:ultra high energy cosmic rays, gamma ray bursts
fermi acceleration
4. ¥¢¥Ö¥¹¥È¥é¥¯¥È:
Ķ¹â¥¨¥Í¥ë¥®¡¼±§ÃèÀþ¡Ê100Eev¤ò±Û¤¨¤ë¥¨¥Í¥ë¥®¡¼¤ò»ý¤Ä¡Ë¤Ï
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5. »²¹Íʸ¸¥ :Hillas Ann. Rev. Astron. Astrophys. 22, 425 (1984)
E. Waxman Phys. Rev. Lett. 75, 386 (1995)
E. Waxman astro-ph/9612061 etc.
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Å·ÂÎʪÍý³ØÉôÌç ±§ÃèʪÍý³Ø¸¦µæ¼¼ £Í£±
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2.Anisotropies in Cosmic Microwave Background: an Analitic Apploach
3.cosmology, CMB anisotropies, Analytic apploach
4.
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5.
W.Hu & N.Sugiyama Apj.444,489(1995)
W.Hu & N.Sugiyama Phys.Rev.D 51,2599(1995)
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K.D.Kokkotas and B.F.Schutz MNRAS 255 119
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E.Seidel Phys. Rev. D. 42 1884
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£µ¡¥È¯É½¤Î¤¿¤á¤Ë¼ç¤ËRefer¤·¤¿ÏÀʸ
R.B.Mann and U.Sarkar DAMTP/R-95/28 (1997)
M.Gasperini Phys.Rev.D38 (1988)
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Large-scale cosmic microwave background
temperature fluctuations are calculated
for a noncompact multiconnected
hyperbolic universe. The mode expansion is
carried out by using Selberg trace formula.
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1.¾®»³Çî»Ò
̾¸Å²°Âç³ØÍý³Ø¸¦µæ²ÊCG¸¦ M1
2.Relativistic plasmas near a Schwarzschild blacck hole:
A solution of the two fluid ODE's in Schwarzschid coordinates
3.relativistic plasma,two-stream instability,jet
4.
³èÆ°¶ä²ÏÃæ¿´³Ë(AGN)¤Ï¤½¤³¤«¤éÊü¼Í¤µ¤ì¤ëËÄÂç¤Ê¥¨¥Í¥ë¥®¡¼¤«¤é¡¢¤½¤ÎÃæ¿´
¤Ë¤ÏĶ¼ÁÎ̤Υ֥é¥Ã¥¯¥Û¡¼¥ë¤¬Â¸ºß¤¹¤ë¤È¹Í¤¨¤é¤ì¤Æ¤¤¤ë¡£Æ±»þ¤ËAGN¤Ï¸÷®
¤Ë¶á¤¤¥¸¥§¥Ã¥È¤¬È¼¤¦¤Î¤¬¤Ò¤È¤Ä¤ÎÆÃħ¤Ç¤¢¤ë¡£Æäˤ½¤Î²Ã®µ¡¹½¤¬¤Þ¤À̤²ò
·è¤ÎÌäÂê¤È¤·¤Æ»Ä¤Ã¤Æ¤¤¤ë¡£¤½¤³¤Ç²æ¡¹¤Ï¥Ö¥é¥Ã¥¯¥Û¡¼¥ë¤¬¤Î¶¯½ÅÎϤˤè¤Ã¤Æ
½¸¤á¤ì¤é¤ì¤¿Â¿Î̤Υץ饺¥ÞÃæ¤Ë¤ª¤±¤ëÇÈÆ°¤ËÃåÌܤ¹¤ë¡£¶ñÂÎŪ¤Ë¤ÏSchwarz-
schild BH »þ¶õÃæ¤Ç¤Î¥×¥é¥º¥Þ¤Î2ήÂÎÊýÄø¼°¤òÍѤ¤¤Æ²òÀϤ·¤¿ÏÀʸ¤ò¾Ò²ð¤·¡¢
¥¤¥ª¥ó-ÅŻҴ֤⤷¤¯¤Ï¥Ý¥¸¥È¥í¥ó-ÅŻҴ֤ËÀ¸¤¸¤ë2ήÂÎÉÔ°ÂÄêÀ¤¬Î³»Ò(ÅÅ»Ò)
²Ã®¤Î¥á¥«¥Ë¥º¥à¤Ë´óÍ¿¤¹¤ë²ÄǽÀ¤¬¤¢¤ë»ö¤ò¸«¤ë¡£
5. V.Buzzi,K.C.Hines,and R.A.Treumann,Phys.Rev.D 51,6663(1995)
V.Buzzi,K.C.Hines,and R.A.Treumann,Phys.Rev.D 51,6677(1995)
V.Buzzi and K.C.Hines,Phys.Rev.D 51,6692(1995)
£±¡¥´Ý»³Àµ¼£¡¡ÂçºåÂç³ØÂç³Ø±¡Íý³Ø¸¦µæ²Ê±§ÃèÃϵå²Ê³ØÀ칶½¤»Î£±Ç¯
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¡¡¡¡¥¤¥ó¥Õ¥ì¡¼¥·¥ç¥ó¤Ë¤Ä¤¤¤Æ³µÀ⤹¤ë¡£
¡¡¡¡¥¤¥ó¥Õ¥ì¡¼¥·¥ç¥ó¤Ë¤ª¤±¤ëÎ̻Ҿì¤òÈóÊ¿¹Õ¤Ê¾ì¤È¤·¤Æ¼è¤ê°·¤¦¤È¡¢system field¤È
¡¡¡¡environment field ´Ö¤ÎÈóÀþ·Á¤ÊÁê¸ßºîÍѤ«¤é colored noise ¤¬¤Ä¤¯¤é¤ì¤ë¡£¤³¤Î
¡¡¡¡colored noise ¸»¤ò¹Í¤¨¤ë¤³¤È¤Ë¤è¤Ã¤Æ¡¢È󥬥¦¥¹Ê¬ÉÛ¤·¤¿¶ä²Ï¤Î·ÁÀ®¤Ë¤Ä¤¤¤Æ
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£µ¡¥Quantum Origin of Noise and Fluctuations in Cosmology
B.h.Hu
Invited talk delivered by B.L.Hu at the Conference on
The Origin of Structure in the Universe
gr-qc/9512049
£± ºÙ¾ÂÀµÌ÷¡Ê¤Û¤½¤Ì¤Þ ¤Þ¤µ¤ä¤¹¡Ë
¹ÅçÂç³ØÍý³ØÉô±§ÃèʪÍý³Ø¸¦µæ¼¼ M£±
£² Black hole area in Brans-Dicke theory
£³ Brans-Dicke theory,area theorem
£´ ½ÅÎϾì¤òÎ̻Ҳ½¤¹¤ëÍýÏÀ¤«¤é¡¢Einstein¤Î½ÅÎϾì¤ÎÍýÏÀ¤Ïscalar¾ì¤ò´Þ¤à¤è¤¦
³ÈÄ¥¤µ¤ì¤ë¤Ù¤¤Ç¤¢¤ë¡¢¤È¤Î·ëÏÀ¤¬½Ð¤µ¤ì¤Æ¤¤¤ë¡£¤³¤³¤Ç¼è¤ê¾å¤²¤ëBrans-
DickeÍýÏÀ¤Ï¾å½Ò¤Î¤è¤¦¤Ê¥¢¥×¥í¡¼¥Á¤«¤é½Ð¤µ¤ì¤¿¤â¤Î¤Ç¤Ï¤Ê¤¤¤¬¡¢scalar¾ì
¤ò´Þ¤à½ÅÎϾì¤ÎÍýÏÀ(scalar-tensorÍýÏÀ)¤ÎºÇ¤âñ½ã¤Ê¤â¤Î¤Ç¤¢¤ê¡¢¼Â¸³Åª¸¡
¾Ú¤ò¼õ¤±¤¿ÍýÏÀ¤Ç¤â¤¢¤ë¡£º£²ó¤ÏBrans-DickeÍýÏÀ¤Î²¼¤Ç¤Îblack hole¤Î¿¶Éñ
¤¤¡¢¥¨¥ó¥È¥í¥Ô¡¼¤Ë¤Ä¤¤¤ÆGungwon Kang¤Ë¤è¤ëÏÀʸ¤òÃæ¿´¤Ë¤·¤Æ¾Ò²ð¤¹¤ë¡£
£µ referrence
Gungwon Kang Phys.Rev. D54 7483 (1996)
T.Jacobson,G.Kang and R.C.Myers Phys.Rev. D49 6587 (1994)
M.A.Scheel,S.L.Shapiro and S.A.Teukolsky Phys.Rev. D51 4238,4208 (1993)
£± µÜÆâ ¸¬ÂÀ¡Ê¤ß¤ä¤¦¤Á ¤±¤ó¤¿¡Ë
¹ÅçÂç³ØÍý³ØÉô±§ÃèʪÍý³Ø¸¦µæ¼¼ M£±
£² Microlensing of Quasars By Stars In Their Damped Ly¦Á Absorbers
£³ Microlensing,Quasars,Damped Ly¦Á Absorbers
£´ QSO¤ÎDamped Ly¦Á AbsorbersÃæ¤ËMicrolensing¤ò°ú¤µ¯¤³¤¹¤è¤¦¤Ê¾®Å·ÂÎ
¤¬Â¸ºß¤¹¤ë¤È¤¹¤ì¤Ð¡¢QSO¤ÎÌÀ¤ë¤µµÚ¤Ó¥¹¥Ú¥¯¥È¥é¥à¤Ë»þ´ÖÊѲ½¤¬µ¯¤³¤ë¤È
´üÂÔ¤µ¤ì¤Æ¤¤¤ë¡£ ¤³¤³¤Ç¤ÏRosalba Perna ¤ÈAbraham Loeb¤ÎÏÀʸ¤ò¾Ò²ð¤¹¤ë¡£
£µ referrence
Rosalba Perna,Abraham Loeb 1997 ApJ in press preprint astro-ph/9701226
ÌðÌîÂÀÊ¿
ÂçºåÂç³ØÍý³ØÉô±§Ãè¿Ê²½
D£²
Stability of scale-invariant cosmological correlation function
in the strongly non-linear clustering regime
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²æ¡¹¤ÏÈóÀþ·ÁÎΰè¤Ç¤ÎÌ©ÅÙÍɤ餮¤Î£²ÂÎÁê´Ø´Ø¿ô¤Ë¤¿¤¤¤¹¤ëBBGKYÊýÄø¼°¤Î
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¤½¤Î¡¢ÈóÀþ·ÁÎΰè¤Ç¤ÎÌ©ÅÙÍɤ餮¤Î£²ÂÎÁê´Ø´Ø¿ô¤Ë¤¿¤¤¤¹¤ëBBGKYÊýÄø¼°¤Î
¶Ò§²ò¤Î°ÂÄêÀ¤òÀÝÆ°¤Î¿¶Éñ¤¤¤ò¸«¤ë¤³¤È¤Ë¤è¤êÄ´¤Ù¤¿¡£
®ÅÙ¶õ´Ö¤Î¥¹¥¥å¡¼¥Í¥¹¤¬¤Ê¤¤»þ¤Ë¤ÏÈóÀþ·ÁÎΰè¤Ç¤Î¥í¡¼¥«¥ë¤ÊÉÔ°ÂÄêÀ¤Ï
¸ºß¤·¤Ê¤¤¤³¤È¤¬¤ï¤«¤Ã¤¿¡£ÀÝÆ°¤ÏÀ®Ä¹¤â¤»¤º¡¢¸º¿ê¤â¤·¤Ê¤«¤Ã¤¿¡£
¤Ä¤Þ¤ê¡¢¥Þ¡¼¥¸¥Ê¥ë¤Ê°ÂÄêÀ¤ò¤â¤Ä¤³¤È¤¬¤ï¤«¤Ã¤¿¡£
¤³¤Î·ë²Ì¡¢²ò¤Î°ÂÄêÀ¤È¤¤¤¦´ÑÅÀ¤«¤é¤¹¤ë¤È£²ÂÎÁê´Ø´Ø¿ô¤Î
¥Ñ¥ï¡¼¥¤¥ó¥Ç¥Ã¥¯¥¹¤Ë´Ø¤·¤ÆÆÃÊ̤ÊÃͤϤʤ¤¤³¤È¤¬¤ï¤«¤Ã¤¿¡£
¤Ä¤Þ¤ê¡¢°ÂÄêÀ¤ÎµÄÏÀ¤«¤é¶¯¤¤ÈóÀþ·ÁÎΰè¤Ç¤Î£²ÂÎÁê´Ø´Ø¿ô¤Î
¥Ñ¥ï¡¼¥¤¥ó¥Ç¥Ã¥¯¥¹¤ò·è¤á¤ë¤³¤È¤Ï¤Ê¤¤¤³¤È¤¬¤ï¤«¤Ã¤¿¡£
Davis,M &Peebles,P.J.E.1977,ApJS,34,425
Ruamsuwan,L. & Fry,J.N.1992,ApJ,396,416
Yano,T. & Gouda, N.1997,ApJ in press
£±¡¤Âçµ×ÊÝ¡¡½¨½Ó¡¤¡¡Áá°ðÅÄÂç³Ø¡ÊÁ°Åĸ¦¡Ë¡¤£Í£²
£²¡¤Ä¶¤Ò¤â±§ÃèÏÀ¤È±§Ãè¤ÎÆðÛÅÀ
£³¡¤¥¬¥¦¥¹-¥Ü¥ó¥Í¹à¡¤¥Ç¥£¥é¥È¥ó¾ì¡¤¥â¥¸¥å¥é¥¤¾ì
£´¡¤¥¢¥¤¥ó¥·¥å¥¿¥¤¥ó¤Î°ìÈÌÁêÂÐÀÍýÏÀ¤Ë½¾¤¦¸Â¤ê±§Ãè½é´ü¤Î
ÆðÛÅÀ¤ÏÈò¤±¤é¤ì¤Ê¤¤¤³¤È¤Ï£Ó¡¥¥Û¡¼¥¥ó¥°¡¤£Ò¡¥¥Ú¥ó¥í¡¼¥º
¤Ê¤É¤Î¡ÖÆðÛÅÀÄêÍý¡×¤Ë¤è¤Ã¤Æ¼¨¤µ¤ì¤¿¡¥¡¡±§Ãè½é´ü¤ò¹Í¤¨¤ë
¤Ë¤Ï½ÅÎϤÎÎÌ»ÒÏÀ¤¬É¬Íפˤʤ롥¡¡¤½¤³¤ÇÅý°ìÍýÏÀ¤È¤·¤ÆÍÎÏ
»ë¤µ¤ì¤Æ¤¤¤ë¡ÖĶ¤Ò¤âÍýÏÀ¡×¤Î£±¥ë¡¼¥×¤ÎÎÌ»ÒÊäÀµ¤Þ¤Ç¤Î¸ú²Ì
¤ò¼è¤êÆþ¤ì¤¿ÍýÏÀ¤Ç±§Ãè½é´ü¤ÎÆðÛÅÀ¤¬Èò¤±¤é¤ì¤ë¤«¤É¤¦¤«¤È
¤¤¤¦¤³¤È¤òÄ´¤Ù¤¿ÏÀʸ¤ò¾Ò²ð¤¹¤ë¡¥
£µ¡¤I.Antoniadis,J.Rizos and K.Tamvakis
Nuclear Physics B415 497-514
R.Easther and K.Maeda Physical Review D 54 7252
£±¡¥Ã«¸ý·É²ð
µþÅÔÂç³ØÍý³ØÉôʪÍýÂèÆ󶵼¼Å·Âγ˸¦µæ¼¼ D£²
£²¡¥Solving the Darwin problem in the first post-Newtonian approximation
of general relativity
£³¡¥post-Newtonian¡¢binary neutron stars¡¢Darwin problem¡¢
innremost stable circular orbit
£´¡¥We analytically calculate the equilibrium sequence of the corotating
binary stars of incompressible fluid in the first post-Newtonian(PN)
approximation of general relativity. By calculating the total energy
and total angular momentum of the system as a function of the
orbital separation, we investigate the innermost stable circular
orbit for corotating binary(we call it ISCCO). It is found that by
the first PN effect, the orbital separation of the binary at the
ISCCO becomes small with increase of the compactness of each star,
and as a result, the orbital angular velocity at the ISCCO
increases. These behaviors agree with previous numerical works.
£µ¡¥K.Taniguchi and M.Shibata, to appear in Phys. Rev. D (1997).
£±¡¥»á̾¡¢½ê°¡¢³Øǯ
²Ï°æ ¿²ð¡¢ µþÅÔÂç³ØÂç³Ø±¡¿Í´Ö´Ä¶³Ø¸¦µæ²Ê¡¢D1
£²¡¥È¯É½¥¿¥¤¥È¥ë
Stability of non-singular universe
£³¡¥È¯É½ÆâÍƤ˴ؤ¹¤ë¥¡¼¥ï¡¼¥É
singularity, Gauss-Bonnet, perturbation
£´¡¥È¯É½ÆâÍƤΥ¢¥Ö¥¹¥È¥é¥¯¥È ¡¡¡ª¡ªÃí°Õ¡ª¡ª¡Ê35ʸ»úx12¹Ô°ÊÆâ¡Ë
There are cosmological non-singular solutions for equation of motion
derived from superstring-based effective action. In this talk,
stability of these solutions and evolution of perturbation are
discussed using gauge-invariant method.
£µ¡¥È¯É½¤Î¤¿¤á¤Ë¼ç¤ËRefer¤·¤¿ÏÀʸ
Antoniadis, Rizos and Tamvakis, Nucl.Phys.B415 497
Wetterich, Nucl.Phys. B324 141
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M1
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Geon ¤È¤Ï²¿¤«
£³¡¥È¯É½ÆâÍƤ˴ؤ¹¤ë¥¡¼¥ï¡¼¥É
geon = gravitational-electromagnetic entity
£´¡¥È¯É½ÆâÍƤΥ¢¥Ö¥¹¥È¥é¥¯¥È
1950ǯÂå¤Ë¡¢¸ÅŵŪ¤ÇÁêÂÐÏÀŪ¼è¤ê°·¤¤¤òɬÍפȤ¹¤ë¤è¤¦¤Ê¤â¤Î¤ÎÎã¤È¤·¤Æ¡¢
Geon¤¬¹Í°Æ¤µ¤ì¤Æ¤¤¤ë¡£¤³¤ì¤Ï¡¢¤¢¤ëÎΰè¤Ë½ÅÎÏŪ¤Ë«Çû¤µ¤ì¤¿Åż§¾ì¤Ç¡¢¤³
¤ÎÅż§¾ì¤ò«Çû¤·¤Æ¤¤¤ë½ÅÎϾì¤Ï¡¢Åż§¾ì¼«¿È¤Î energy-momoentum tensor
¤ò¸»¤È¤¹¤ë¤â¤Î¤Ç¤¢¤ë¡£¤³¤Î geon ¤¬Â¸ºß¤¹¤ë¤È¤·¤¿¤È¤¤Î¿¶Éñ¤¤¤òÄ´¤Ù¤¿¡£
¤¿¤À¤·¡¢Åż§¾ì¤ÎʬÉۤȤ·¤ÆµåÂоÎÀÅŪ¤Ê¤â¤Î¤ò²¾Äꤷ¤¿¡£
£µ¡¥È¯É½¤Î¤¿¤á¤Ë¼ç¤ËRefer¤·¤¿ÏÀʸ
Phys.Rev. 97 (1954) 511-536 J.A.Wheeler "Geons"
£±¡¥»á̾ °æÅÄ ÂçÊå
½ê° µþÅÔÂç³Ø Íý³Ø¸¦µæ²Ê ʪÍý³ØÂèÆ󶵼¼ Å·Âγ˸¦µæ¼¼¡£
³Øǯ ½¤»Î£²
£²¡¥È¯É½¥¿¥¤¥È¥ë Kastor-Traschen »þ¶õ¤ÎEvent Horizon¤ÈHoop Conjecture
£³¡¥È¯É½ÆâÍƤ˴ؤ¹¤ë¥¡¼¥ï¡¼¥É Kastor-Traschen solutions, black holes
collision, hoop conjecture
£´¡¥È¯É½ÆâÍƤΥ¢¥Ö¥¹¥È¥é¥¯¥È
Kastor-Traschen²ò¤ÏCosmological Einstein-Maxwell·Ï¤Î¸·Ì©²ò¤Ç¤¢¤ê¡¢
Ǥ°Õ¸Ä¤Î²ÙÅÅ¥Ö¥é¥Ã¥¯¥Û¡¼¥ë¤Î¾×Æͤòµ½Ò¤¹¤ë¡£
²æ¡¹¤Ï£²¤Ä¤ÎÅù¼ÁÎ̤Υ֥é¥Ã¥¯¥Û¡¼¥ë¤¬¾×Æͤ¹¤ë¾ì¹ç¤Ë¤Ä¤¤¤Æ¡¢¤³¤Î»þ¶õ¤Î
Event Horizon¤ò¿ôÃÍŪ¤Ëµá¤á¤¿¡£
¤µ¤é¤Ë¡¢Event Horizon¤òÀ¸À®¤¹¤ënull generator¤Îpast endpoints¤«¤é¤Ê¤ë½¸
¹ç¤òÄ´¤Ù¤¿¤È¤³¤í̵¸Â¤ËŤ¤¶ÊÀþ¤Ç¤¢¤Ã¤¿¤¬¡¢¤³¤Î¤³¤È¤¬hoop conjecture¤ËÂÐ
¤·¤Æ¤É¤Î¤è¤¦¤Ê¼¨º¶¤òÍ¿¤¨¤ë¤«¤Ë¤Ä¤¤¤ÆµÄÏÀ¤¹¤ë¡£
£µ¡¥È¯É½¤Î¤¿¤á¤Ë¼ç¤ËRefer¤·¤¿ÏÀʸ
£±¡¥¡Ê»á̾¡¢½ê°¡¢³Øǯ¡Ë
À¾Ûê ÅýÇ·
Áá°ðÅÄÂç³ØÂç³Ø±¡ Íý¹©³Ø¸¦µæ²Ê ʪÍý³ØµÚ±þÍÑʪÍý³ØÀ칶
Å·ÂÎʪÍý³ØÉôÌç ±§ÃèʪÍý³Ø¸¦µæ¼¼ £Ä£±
£²¡¥¡Êȯɽ¥¿¥¤¥È¥ë¡Ë
Spin effect on gravitational radiation
£³¡¥¡ÊȯɽÆâÍƤ˴ؤ¹¤ë¥¡¼¥ï¡¼¥É¡Ë
Gravitational radiation, Gravitational waveform,
Black hole perturbation approach, Spinning test
particle
£´¡¥¡ÊȯɽÆâÍƤΥ¢¥Ö¥¹¥È¥é¥¯¥È¡Ë
We consider a spinning test particle moving on an
equatorial plane of Kerr black hole and calculate its
total emitted energy, total angular momentum, energy
spectrum, and gravitational waveform of gravitational
radiation. First, we find that the total emitted energy
largely depends on (so called) spin-orbit coupling
effect. Second, we can see from the energy spectrum that
when the particle spin becomes anti-parallel to the
black hole spin, the m=l mode spectrum supresses and the
m=l-1 mode enhances. Therefore, gravitational waveform
becomes complicated. The quasi-normal mode frequency is
the most promissing part of detecting gravitational
wave, there are some cases that the ringing tail part of
gravitational wave little oscillates because of the
spin-spin cancellation effect.
£µ¡¥¡Êȯɽ¤Î¤¿¤á¤Ë¼ç¤ËRefer¤·¤¿ÏÀʸ¡Ë
S. A. Teukolsky, Astrophys. J. 185, 635 (1973).
S. Chandrasekher, The Mathematical Theory of Black Holes
(Oxford University Press, 1983).
T. Nakamura, K. Oohara, and Y. Kojima, Prog. Theor.
Phys. Suppl. 90, 110 (1987).
W. G. Dixon, Isolated Gravitating Systems in General
Relativity, edited by J. Ehlers (North-Holland,
Amsterdam, 1979), p.156.
Y. Mino, M. Shibata and T. Tanaka, Phys. Rev. D 53, 622
(1996).
T. Tanaka, Y. Mino, M. Shibata and M. Sasaki, Phys. Rev.
D 54, 3762 (1996).
£±¡¥Ã«¡¡Ä¾¼ù¡Êntani@th.phys.titech.ac.jp¡Ë¡¢ºÙ롦Àи¶¸¦¡¢£Í£²
£²¡¥de Sitter»þ¶õ¤Ë¤¢¤ë¥Ö¥é¥Ã¥¯¥Û¡¼¥ë¤Î°ÂÄêÀ¡Ê²¾¡Ë
£³¡¥quasinormal mode¡¢Cauchy horizon
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¡¡¡¡Reissner-Nordstrom¥Ö¥é¥Ã¥¯¥Û¡¼¥ë¤Î°ÂÄêÀ¤òÄ´¤Ù¤ë¡£
¡¡¡¡¤³¤Î»þ¶õ¤Ë¤¢¤ëCauchy horizon¤Ï¡¢¾ì¤ÎÀÝÆ°¤ËÂФ·°ÂÄê¤Ç¤¢¤ë¤³¤È¤¬È½
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£µ¡¥Felicity Mellor and Ian Moss,PHYSICAL REVIEW D,VOLUME41
,NUMBER2(1990)
£±¡¥°æ²¬Ë®¿Î¡¢µþÅÔÂç³ØʪÍý³Ø¶µ¼¼±§ÃèÊü¼Í³Ø¡ÊÍýÏÀ¡ËM£±
£²¡¥È¯É½¥¿¥¤¥È¥ë¡¡MACHOs¤Ë´Ø¤·¤Æ
£³¡¥È¯É½ÆâÍƤ˴ؤ¹¤ë¥¡¼¥ï¡¼¥É¡¡MACHO,gravitational lens,dark matter
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a counter example of cosmic cencership hypothesis. To investigate the
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