|
我国物理学家陈绍光在第36届世界空间科学大会上作报告：用广义相对论推导出奇性黑洞不存在。 陈绍光在COSPAR2006 的E1.2/H0.2-2专题中作报告指出: 由于爱因斯坦方程是非线性方程, 遵从广义相对论的引力不满足线性迭加原理, 使得无论多大的中子星其内部的引力都不可能超过中子气的简并压力, 因此无限大密度与无限大引力的奇性黑洞不可能产生。中子星内部是一个对外无任何信息交流尤其是对外无引力作用的黑洞，中子星的形成就表现为引力质量的损失或负引力(或反引力)的出现,被称为暗物质与暗能量现象实质上是就是爱因斯坦方程是非线性效应。 详见论文：COSPAR2006-A-00624；E1.2-0040-06 |
|
论文：Black hole inside neutron stars caused by nonlinear effect of Einstein’s equation Black hole inside neutron stars caused by nonlinear effect of Einstein’s equation Chen Shao-Guang Institute of Physics, Academy of Sciences-Jiangxi, P.R.China Email: ch503en @ 163.com , According to the variance in mass of inductive gravitation deduced by H.Bondi from general relativity〔H. Bondi, Proc. R. Soc. London A 427,249 (1990)〕and the definition of force f ≡ δ(m v)/δt ＝m(δv/δt )＋v(δm/δt ) a new gravitational formula was obtained: f ≡ δ(m v)/δt ＝f P ＋ f C ＝ －G(m M / r 2 ) (r/r)－G(m M / r 2 ) (v/c) (1) f P ＝m(δv/δt ) is produced by the rate of variance in velocity v when the mass m is invariable. Because Newtonian gravitation law is included in the general relativity (GR), when not partial-difference for m, the mass m is invariable, it implies that the mass may produce the gravitational field but the gravitational field should not lead to the variance in mass. i.e., the mass m should be an invariable parameter and the fourth dimension momentum m c (or energy m c 2 ) should be entirely independence on three-dimension momentum m v. In other words, the energy and the momentum should not compose the four-dimension momentum-energy vector and tensor. So, the gravitational equation should change into linear from nonlinear, and Einstein’s equation should degenerate into Newtonian law: f P ＝m(δv/δt ) ＝ －G(m M / r 2 ) (r/r) f C ＝v(δm/δt ) is produced by the rate of variance in mass when the velocity v is invariable. First according to the mass-energy relationship in special relativity we getδm /δt ＝δE /c2δt , again from the conservation of four dimension momentum–energy vector P–E in special relativity, we getδE /δt ＝c δ∣P ∣/δt, so f C ＝v(δm/δt ) ＝vδ∣P ∣/c δt ＝vδP /c δt ＝v f P /c＝－G(m M / r 2 ) (v/c) Eq.(1) is equivalent to Einstein’s equation, then, the multi-bodies gravitational problems now can be strictly solved. f C embodies the tangled interaction between field and source and causes un-modeled acceleration of Pioneer 10/11. Eq.(1) can directly be tested by the absolutely measure the gravitational acceleration in vacuum with long falling pipe or projection method. The variance in mass of Bondi’s inductive gravitation caused by body B appears nearby body A. When third body C appears nearby bodies A and B, the original masses of A and B will change, the original force f between A and B will also changes. Whether v＝0 or v≠0, the variance in mass of Bondi’s inductive gravitation always leads to that the gravitation f dissatisfies the linear superposition principle. This is an essential character of gravitation described by nonlinear Einstein’s equation and to be called as gravitation shielding effect. For the self shielding effect the mass M of non-mass-point corrects to M (1－q ), q is a positive shielding coefficient : f ＝－G∞ m M (1－q ) r / r 3 ＝－G (r ) m M r / r 3 (2) G (r）＝G∞(1－q ), q ＝KΕ ＝K M/ r 2 ＝KρL S/ r 2＝KρLΩ , G∞ is the gravitational constant of mass-point, E the gravitational field strength, ρ 、L、S the density、thickness、cross section of M respectively, Ω the solid angle of M subtends to m, K is an experimental constant as a section of unit mass. Numerous experimental and observational results such as “gravitation abnormality”during eclipse、“fifth kind force”etc had been explained by Eq. (2). From the average value q ＝1.6×10-13 m-1 measured by F. D. Stacey et al、Q.Majorana etc we get atomic Katom＝9.4×10-14 m2 kg-1.〔Chen Shao-Guang , Nuovo Cimento B 104, 611 (1989)〕. Because of the de. Bloglie wavelength and section of electrons far large than that of nucleons, convert to nucleonic Knucl.＝4.7×10-20 m2 kg-1. For a neutron star sphere shell ρ ＝6×1017kgm-3, Ω ＝4π, according to Eq. (2) and Knucl, when L＝3m, q ＝1, it can completely isolate the gravitational interaction between inner layer and outside layer. From the experimental sectionσ＝1×10-47m2 of single nucleon to neutrinoνe we get Kνe ＝1.0×10-21 m2 kg-1, when L＝130m, q ＝1 in Eq. (2), it can completely block off the neutrinos. A neutron star layer of 1km thickness can completely isolate the gravity and information communion via neutrinos and photons, only most-exterior shell of 1km thickness has interaction on the outside world (as an empty spherical shell). Once neutron star come into being, its bosom becomes as a black hole without gravity and violates the equilibrium between Newtonian gravity and centrifugal force in the galaxies, it represents as the phenomena of “dark matter”and“dark energy”. The maximal gravity inside neutron stars is produced only by the masses of a sphere in radius of 1km, it is impossible that the gravity larger than the pressure of degenerate neutron gas, the neutron stars cannot further collapse into singularity point with infinite density. Therefore, the neutron stars has no upper limit of mass, it can exceed 3M⊙ and could be reach 150 M⊙ indeed several thousands or several millions M⊙ . A black hole with infinite gravity could be formed only for Newtonian gravitational law which satisfies the linear superposition principle but not for nonlinear Einstein’s equation. Otherwise, the necessary rest and isolation condition of spherical symmetry metric such as Schwarzschild’s metric and Kerr’s metric, makes the black holes derived from metric have not matter around it , then, has no gravitational interaction to the outsid |
|
口头报告程序：Oral Programme - E1.2/H0.2-2 Multi-scale and Multi-wavelength Studies of Black Holes Oral Programme - E1.2/H0.2-2 Multi-scale and Multi-wavelength Studies of Black Holes Please, click Abstract Number to find the corresponding abstract as PDF file; if necessary, download Adobe Acrobat Reader 4.0 first to open the file. Any abstract may be freely reproduced for non-commercial, scientific purposes; however, the moral right of the author(s) to be identified as the author(s) of such abstracts is asserted. MSO: Li, T. DO: Mirabel, F. Co-Sponsorship: Wednesday, 19 July 2006 Lecture Room: 405-406 Chairperson: MIRABEL,F. 9:30 - 9:50 COSPAR2006-A-01047; E1.2-0001-06 Zakharov, A.; DePaolis, F.; Nucita, A.; Ingrosso, G. Studies of signatures of black hole existence with space missions (solicited) 9:50 - 10:20 COSPAR2006-A-03064; E1.2-0002-06 Zhao, P; Grindlay, J; Hong, J; Laycock, S; Koenig, X; van den Berg, M Chandra Multiwavelength Plane (ChaMPlane) Survey (solicited) 10:20 - 10:50 COSPAR2006-A-03073; E1.2-0003-06 Bouchet, L.; THE SPI/INTEGRAL TEAM Study of black holes population with SPI/INTEGRAL (solicited) 10:50 - 10:53 COSPAR2006-A-01326; E1.2-0004-06 Biryukov, A.; Beskin, G.; Karpov, S. Observational appearances of isolated stellar-mass black hole accretion - theory and observations. 10:53 - 10:54 COSPAR2006-A-00054; E1.2-0005-06 Kryvdyk, V. Collapse of stars to black holes: from theory to observations 10:54 - 11:04 Discussion 11:04 COFFEE BREAK Chairperson: ZDZIARSKI,A.A. 11:30 - 11:55 COSPAR2006-A-02356; E1.2-0006-06 de Gouveia Dal Pino, E. M.; Lazarian, A. The role of magnetic reconnection on accretion phenomena associated to black holes (solicited) 11:55 - 12:05 COSPAR2006-A-00052; E1.2-0007-06 Kryvdyk, V. Formation of the relativistic jets by collapse star to black hole 12:05 - 12:20 COSPAR2006-A-03081; E1.2-0008-06 Joinet, A. ; SPI/INTEGRAL TEAM GX339-4 and H1743-322 observed by SPI/INTEGRAL during a state transition 12:20 - 12:40 COSPAR2006-A-02940; E1.2-0009-06 Mendez, M. Relativistic emission line or warm absorber in GRS 1915+105 (solicited) 12:40 - 13:05 COSPAR2006-A-01396; E1.2-0010-06 Casella, P.; Belloni, T.; Homan, J.; Stella, L.; van der Klis, M. Low-frequency QPOs in X-ray binaries: fundamental physics at work (solicited) 13:05 - 13:07 COSPAR2006-A-00998; E1.2-0011-06 Liu, J; Di Stefano, R.; Kong, A.; Primini, F.; Bregman, J. Discovery of an X-ray binary with a 22.45 hour period in M101 13:07 - 13:17 Discussion 13:17 LUNCH BREAK Chairperson: MENDEZ,M.;LIANG,E. 15:30 - 15:50 COSPAR2006-A-02438; E1.2-0012-06 Zdziarski, A. A.; Gierlinski, M. Energy-dependent timing properties of black-hole binaries (solicited) 15:50 - 16:10 COSPAR2006-A-02095; E1.2-0013-06 Yu, W Black hole mass, accretion geometry and state transitions in black hole binaries (solicited) 16:10 - 16:25 COSPAR2006-A-00689; E1.2-0014-06 Liang, E; Boettcher, M Numerical simulations of black hole emissions and transitions 16:25 - 16:55 COSPAR2006-A-01138; E1.2-0015-06 Cheng, K.S.; Chernyshov, D.O.; Dogiel, V.A. Annihilation emission from the galactic black hole (solicited) 16:55 - 17:05 COSPAR2006-A-00592; E1.2-0016-06 Y., Lu; Y.F., Huang; S.N., Zhang A constrain on the radiation efficiency of stellar disruption by a massive black hole 17:05 - 17:30 COSPAR2006-A-02643; E1.2-0017-06 Soria, R. Revising our view of ultraluminous X-ray sources (solicited) 17:30 - 17:55 COSPAR2006-A-01719; E1.2-0018-06 Shen, Z.-Q.; Huang, L.; Cai, M. Black hole shadow image and its application in visibility analysis of Sgr A* (solicited) 17:55 - 18:05 COSPAR2006-A-02161; E1.2-0019-06 Miyazaki, A.; Shen, Z.-Q.; Miyoshi, M.; Tsutsumi, T.; Tsuboi, M. Flux variations of Sagittarius A* at short millimeter wavelengths 18:05 - 18:30 COSPAR2006-A-02437; E1.2-0020-06 Liu, L; Petrosian, P; Melia, M; Fryer, F Testing the Stochastic Acceleration Model for Flares in Sagittarius A* (solicited) 18:30 END OF THE DAY Thursday, 20 July 2006 Lecture Room: 405-406 Chairperson: BOUCHET,L. 9:30 - 9:55 COSPAR2006-A-01928; E1.2-0021-06 Giovannini, G. ; Giroletti, M. ; Taylor, G.B. ; Falomo, R. Multi-wavelength analysis of a sample of low-redshift BL Lac objects (solicited) 9:55 - 10:10 COSPAR2006-A-00084; E1.2-0022-06 Osone, S. Study of long periodicity for Blazar Mkn501 in 1997 10:10 - 10:20 COSPAR2006-A-00245; E1.2-0023-06 Zhang, Y.H. Multi-wavelength view of TeV blazar PKS 2155-304 with XMM-Newton 10:20 - 10:30 COSPAR2006-A-01674; E1.2-0024-06 Fan, J.; Wang, Y.; Li, J.; Zhou, J. The Black Hole Masses of Blazars 10:30 - 10:55 COSPAR2006-A-02250; E1.2-0025-06 Yuan, W. X-ray properties of high-redshift extreme radio-loud quasars (solicited) 10:55 - 11:10 COSPAR2006-A-01866; E1.2-0026-06 Shen, S.; White, S.; Mo, H.J.; Voges, W.; Kauffmann, G.; Tremonti, C.; Anderson, S.F. The soft X-ray properties of quasars in the Sloan Digital Sky Survey 11:10 COFFEE BREAK Chairperson: ZHAO,P. 11:30 - 11:55 COSPAR2006-A-03045; E1.2-0027-06 Xu, D.; Komossa, S.; Zhou, H.; Wang, T. The dependence of NLR/BLR properties on accretion rate of super massive black holes (solicited) 11:55 - 11:58 COSPAR2006-A-01863; E1.2-0028-06 Bian, W.; Gu, Q.; Zhao, Y. Supermassive Black Holes in Type II Quasars 11:58 - 12:01 COSPAR2006-A-01700; E1.2-0029-06 Chao, L.; Bian, W.; Huang, K. The mass relation between the SMBH and the bulge for NLS1s and BLS1s 12:01 - 12:16 COSPAR2006-A-01671; E1.2-0030-06 Liu, Y; Zhang, S. N.; Zhang, X. L. Relativistic effects on the observed AGN luminosity distribution and spectral shapes of Seyfert galaxies 12:16 - 12:19 COSPAR2006-A-03088; E1.2-0031-06 Huang, Z.-Y.; Chen, L.-W. A multi-wavelength study of X-ray jets in active galaxies 12:19 - 12:22 COSPAR2006-A-03479; E1.2-0032-06 Gong, B.P. An alternative model on super luminous motion of microquasars and quasars 12:22 - 12:52 COSPAR2006-A-02928; E1.2-0033-06 Isobe, N.; Griffiths, R.; Itoh, T.; Anabuki, N.; Awaki, H.; Dewangan, G.; Madejski, G.; Makishima, K.; Okajima, T.; Reeves, J.; Suzaku SWG team of NGC 4945 Suzaku observation of nearby Seyfert 2 galaxy NGC 4945 (solicited) 12:52 - 12:54 COSPAR2006-A-03265; E1.2-0034-06 Ho, P.-L.; Chen, L.-W. A multi-wavelength study of the merger candidate Abell S0721 and the activities of its member galaxies 12:54 - 13:19 COSPAR2006-A-03677; E1.2-0035-06 Mirzoyan, R.; The MAGIC Collaboration The 17m Diameter MAGIC Telescope Project for VHE Gamma Ray Astrophysics (solicited) 13:19 - 13:21 COSPAR2006-A-00179; E1.2-0036-06 Beck-Winchatz, B.; Anderson, S. F. A morphological and multicolor HST survey for faint quasars 13:21 - 13:22 COSPAR2006-A-00411; E1.2-0037-06 Beck-Winchatz, B.; Anderson, S. F. Faint quasar candidates from Hubble Space Telescope imaging: Number counts from high-latitude fields 13:22 - 13:32 Discussion 13:32 LUNCH BREAK Chairperson: CHENG,K.S. 15:30 - 15:45 COSPAR2006-A-03371; E1.2-0038-06 Gomboc, A.; Kostic, U.; Cadez, A.; Calvani, M. The Flares and Spectrum of an Asteroid captured by a Black Hole 15:45 - 15:55 COSPAR2006-A-01034; E1.2-0039-06 Nakis, K. Black Holes & Quantum Information 15:55 - 16:05 COSPAR2006-A-00624; E1.2-0040-06 Chen, S.G Black hole inside neutron stars caused by nonlinear effect of Einstein’s equation 16:05 - 16:08 COSPAR2006-A-01255; E1.2-0041-06 Dyadechkin, S. A.; Semenov, V. S.; Biernat, H. K.; Penz, T. A comparison of magnetic flux tube and cosmic string behavior in Kerr metric 16:08 END OF SESSION |
|
论文接受号：List of Accepted Contributions - E1.2/H0.2-2 Multi-scale and Multi-wavelength Studies of Black List of Accepted Contributions - E1.2/H0.2-2 Multi-scale and Multi-wavelength Studies of Black Holes Please, click Abstract Number to find the corresponding abstract as PDF file; if necessary, download Adobe Acrobat Reader 4.0 first to open the file. Any abstract may be freely reproduced for non-commercial, scientific purposes; however, the moral right of the author(s) to be identified as the author(s) of such abstracts is asserted. COSPAR2006-A-00052 Kryvdyk, V. Formation of the relativistic jets by collapse star to black hole COSPAR2006-A-00054 Kryvdyk, V. Collapse of stars to black holes: from theory to observations COSPAR2006-A-00084 Osone, S. Study of long periodicity for Blazar Mkn501 in 1997 COSPAR2006-A-00179 Beck-Winchatz, B.; Anderson, S. F. A morphological and multicolor HST survey for faint quasars COSPAR2006-A-00245 Zhang, Y.H. Multi-wavelength view of TeV blazar PKS 2155-304 with XMM-Newton COSPAR2006-A-00411 Beck-Winchatz, B.; Anderson, S. F. Faint quasar candidates from Hubble Space Telescope imaging: Number counts from high-latitude fields COSPAR2006-A-00592 Y., Lu; Y.F., Huang; S.N., Zhang A constrain on the radiation efficiency of stellar disruption by a massive black hole COSPAR2006-A-00624 Chen, S.G Black hole inside neutron stars caused by nonlinear effect of Einstein’s equation COSPAR2006-A-00689 Liang, E; Boettcher, M Numerical simulations of black hole emissions and transitions COSPAR2006-A-00998 Liu, J; Di Stefano, R.; Kong, A.; Primini, F.; Bregman, J. Discovery of an X-ray binary with a 22.45 hour period in M101 COSPAR2006-A-01034 Nakis, K. Black Holes & Quantum Information COSPAR2006-A-01047 Zakharov, A.; DePaolis, F.; Nucita, A.; Ingrosso, G. Studies of signatures of black hole existence with space missions COSPAR2006-A-01138 Cheng, K.S.; Chernyshov, D.O.; Dogiel, V.A. Annihilation emission from the galactic black hole COSPAR2006-A-01255 Dyadechkin, S. A.; Semenov, V. S.; Biernat, H. K.; Penz, T. A comparison of magnetic flux tube and cosmic string behavior in Kerr metric COSPAR2006-A-01326 Biryukov, A.; Beskin, G.; Karpov, S. Observational appearances of isolated stellar-mass black hole accretion - theory and observations. COSPAR2006-A-01396 Casella, P.; Belloni, T.; Homan, J.; Stella, L.; van der Klis, M. Low-frequency QPOs in X-ray binaries: fundamental physics at work COSPAR2006-A-01671 Liu, Y; Zhang, S. N.; Zhang, X. L. Relativistic effects on the observed AGN luminosity distribution and spectral shapes of Seyfert galaxies COSPAR2006-A-01674 Fan, J.; Wang, Y.; Li, J.; Zhou, J. The Black Hole Masses of Blazars COSPAR2006-A-01700 Chao, L.; Bian, W.; Huang, K. The mass relation between the SMBH and the bulge for NLS1s and BLS1s COSPAR2006-A-01719 Shen, Z.-Q.; Huang, L.; Cai, M. Black hole shadow image and its application in visibility analysis of Sgr A* COSPAR2006-A-01863 Bian, W.; Gu, Q.; Zhao, Y. Supermassive Black Holes in Type II Quasars COSPAR2006-A-01866 Shen, S.; White, S.; Mo, H.J.; Voges, W.; Kauffmann, G.; Tremonti, C.; Anderson, S.F. The soft X-ray properties of quasars in the Sloan Digital Sky Survey COSPAR2006-A-01928 Giovannini, G. ; Giroletti, M. ; Taylor, G.B. ; Falomo, R. Multi-wavelength analysis of a sample of low-redshift BL Lac objects COSPAR2006-A-02095 Yu, W Black hole mass, accretion geometry and state transitions in black hole binaries COSPAR2006-A-02161 Miyazaki, A.; Shen, Z.-Q.; Miyoshi, M.; Tsutsumi, T.; Tsuboi, M. Flux variations of Sagittarius A* at short millimeter wavelengths COSPAR2006-A-02250 Yuan, W. X-ray properties of high-redshift extreme radio-loud quasars COSPAR2006-A-02356 de Gouveia Dal Pino, E. M.; Lazarian, A. The role of magnetic reconnection on accretion phenomena associated to black holes COSPAR2006-A-02437 Liu, L; Petrosian, P; Melia, M; Fryer, F Testing the Stochastic Acceleration Model for Flares in Sagittarius A* COSPAR2006-A-02438 Zdziarski, A. A.; Gierlinski, M. Energy-dependent timing properties of black-hole binaries COSPAR2006-A-02643 Soria, R. Revising our view of ultraluminous X-ray sources COSPAR2006-A-02928 Isobe, N.; Griffiths, R.; Itoh, T.; Anabuki, N.; Awaki, H.; Dewangan, G.; Madejski, G.; Makishima, K.; Okajima, T.; Reeves, J.; Suzaku SWG team of NGC 4945 Suzaku observation of nearby Seyfert 2 galaxy NGC 4945 COSPAR2006-A-02940 Mendez, M. Relativistic emission line or warm absorber in GRS 1915+105 COSPAR2006-A-03045 Xu, D.; Komossa, S.; Zhou, H.; Wang, T. The dependence of NLR/BLR properties on accretion rate of super massive black holes COSPAR2006-A-03064 Zhao, P; Grindlay, J; Hong, J; Laycock, S; Koenig, X; van den Berg, M Chandra Multiwavelength Plane (ChaMPlane) Survey COSPAR2006-A-03073 Bouchet, L.; THE SPI/INTEGRAL TEAM Study of black holes population with SPI/INTEGRAL COSPAR2006-A-03081 Joinet, A. ; SPI/INTEGRAL TEAM GX339-4 and H1743-322 observed by SPI/INTEGRAL during a state transition COSPAR2006-A-03088 Huang, Z.-Y.; Chen, L.-W. A multi-wavelength study of X-ray jets in active galaxies COSPAR2006-A-03265 Ho, P.-L.; Chen, L.-W. A multi-wavelength study of the merger candidate Abell S0721 and the activities of its member galaxies COSPAR2006-A-03371 Gomboc, A.; Kostic, U.; Cadez, A.; Calvani, M. The Flares and Spectrum of an Asteroid captured by a Black Hole COSPAR2006-A-03479 Gong, B.P. An alternative model on super luminous motion of microquasars and quasars COSPAR2006-A-03677 Mirzoyan, R.; The MAGIC Collaboration The 17m Diameter MAGIC Telescope Project for VHE Gamma Ray Astrophysics |
|
现今流行的黑洞理论的错误在于：用力的线性迭加原理——“质量愈大则引力愈大”来估算中子星的内部引力，没有用非线性的爱因斯坦 现今流行的黑洞理论的错误在于：用力的线性迭加原理——“质量愈大则引力愈大”来估算中子星的内部引力，没有用非线性的爱因斯坦方程直接计算中子星内部的引力，从而得出“大于3个太阳质量（M⊙）的中子星的内部引力会超出中子气的简并压力”这一错误结论。 |
|
黑洞并非是无限大密度与无限大引力 只要该天体的逃逸速度等于光速对应计算出的密度就行。 此时该天体引力也非无穷大，都能计算出具体值。 ※※※※※※ 科学求真；宗教求善；艺术求美 |
|
黑洞是否形成，不完全取决于质量，还和星体半径R有关 从而得出“大于3个太阳质量（M⊙）的中子星的内部引力会超出中子气的简并压力” 还要看半径，或者说要由中子星密度决定。 ※※※※※※ 科学求真；宗教求善；艺术求美 |
|
你的由数学度规的逃逸速度所标记的黑洞不具有物理的真实性
物理学的黑洞是由中子星（物质密度约10^14g/cm^3）坍缩而成, 其密度大于中子星的密度而成为物理学的奇性点, 物理奇点的物质抵抗不了进一步坍缩的引力, 非量子的说法是:中子星将坍缩成一个体积趋于零的点,从而密度和引力将趋于无限大。 你的由数学度规的逃逸速度所标记的黑洞不具有物理的真实性, 因为无论是施瓦兹黑洞还是克尔黑洞都是基于球对称的施瓦兹度规或克尔度规, 这些度规成立的条件是球对称的转动或不转动的孤立物体。当球附近有另一物体存在就成了两体问题，从爱因斯坦方程就求解不出施瓦兹度规和克尔度规, 施瓦兹黑洞和克尔黑洞都会失去了存在条件而不再成立.。使得施瓦兹黑洞和克尔黑洞都不可能有被它们的引力所作用的物体存在，即是说，现今流行的度规理论的黑洞不存在受它作用的客体，从而不可能对外有作用力。既然孤立球体无任何物质质点，说逃逸速度是毫无意义的。总之，现今流行的度规黑洞是孤立球，对外没有引力作用，若说它有对外引力则施瓦兹度规和克尔度规的前提条件不成立，施瓦兹黑洞和克尔黑洞就不可能存在。 |
|
中子星有确定的密度范围, 对于球而言质量确定了半径的范围就确定。从爱因斯坦方程只能求球的解而且必需是孤立的球。 中子星有确定的密度范围, 对于球而言质量确定了半径的范围就确定。从爱因斯坦方程只能求球的解而且必需是孤立的球。 |
|
陈绍光用广义相对论解释了暗物质、暗能量等引力“异常”现象，这对反相、保相两派都不是好消息。保相派对相对论的错误解读使得众 陈绍光用广义相对论解释了暗物质、暗能量等引力“异常”现象，这对反相、保相两派都不是好消息。保相派对相对论的错误解读使得众多的不该出现的引力“异常”如暗物质、暗能量、先峰号飞船的反常加速度等等都出现了並广为流传；反相派正是根据这些引力“异常”现象来质疑和否定相对论。现在保相派若坚持错误的解读则要承担曲解並挖相对论墻脚的罪名，反相派若坚持要推翻相对论则没有了事实依据而且必将面临失败的结束。 |
|
回复:中子星再坍缩后为什么就没有下一级的斥力对抗引力?跨克星不可以么? 我国物理学家陈绍光在第36届世界空间科学大会上作报告：用广义相对论推导出奇性黑洞不存在 |
|
在近代物理这个乱摊里是没有拐棍的,靠哪一个都会陷入沼泽地,最后埋葬自己. 我国物理学家陈绍光在第36届世界空间科学大会上作报告：用广义相对论推导出奇性黑洞不存在 |