ترغب بنشر مسار تعليمي؟ اضغط هنا

Negative Entropy and Black Hole Information

101   0   0.0 ( 0 )
 نشر من قبل Daegene Song
 تاريخ النشر 2013
  مجال البحث فيزياء
والبحث باللغة English
 تأليف Daegene Song




اسأل ChatGPT حول البحث

Based on negative entropy in entanglement, it is shown that a single-system Copenhagen measurement protocol is equivalent to the two-system von Neumann scheme with the memory filling up the system with negative information similar to the Dirac sea of negative energy. After equating the two quantum measurement protocols, we then apply this equivalence to the black hole radiation. That is, the black hole evaporation corresponds to the quantum measurement process and the two evaporation approaches, the observable-based single-system and the two-system entanglement-based protocols, can be made equivalent using quantum memory. In particular, the measurement choice, theta, with the memory state inside the horizon in the entanglement-based scheme is shown to correspond to the observable of the measurement choice, theta, outside the horizon in the single-system protocol, that is, O_{theta}^{out} = Q_{theta}^{in}. This indicates that the black hole as quantum memory is filling up with negative information outside the horizon, and its entropy corresponds to the logarithm of a number of equally probable measurement choices. This shows that the black hole radiation is no different than ordinary quantum theory.



قيم البحث

اقرأ أيضاً

93 - Dongshan He , Qing-yu Cai 2016
When two objects have gravitational interaction between them, they are no longer independent of each other. In fact, there exists gravitational correlation between these two objects. Inspired by E. Verlindes paper, we first calculate the entropy chan ge of a system when gravity does positive work on this system. Based on the concept of gravitational correlation entropy, we prove that the entropy of a Schwarzschild black hole originates from the gravitational correlations between the interior matters of the black hole. By analyzing the gravitational correlation entropies in the process of Hawking radiation in a general context, we prove that the reduced entropy of a black hole is exactly carried away by the radiation and the gravitational correlations between these radiating particles, and the entropy or information is conserved at all times during Hawking radiation. Finally, we attempt to give a unified description of the non-extensive black-hole entropy and the extensive entropy of ordinary matter.
104 - Marco Spaans 2016
Black holes are extreme expressions of gravity. Their existence is predicted by Einsteins theory of general relativity and is supported by observations. Black holes obey quantum mechanics and evaporate spontaneously. Here it is shown that a mass rate $R_fsim 3times 10^{-8} (M_0/M)^{1/2}$ $M_0$ yr$^{-1}$ onto the horizon of a black hole with mass $M$ (in units of solar mass $M_0$) stimulates a black hole into rapid evaporation. Specifically, $sim 3 M_0$ black holes can emit a large fraction of their mass, and explode, in $M/R_f sim 3times 10^7 (M/M_0)^{3/2}$ yr. These stimulated black holes radiate a spectral line power $P sim 2times 10^{39} (M_0/M)^{1/2}$ erg s$^{-1}$, at a wavelength $lambda sim 3times 10^5 (M/M_0)$ cm. This prediction can be observationally verified.
106 - Juan Maldacena 2018
We give a brief overview of black hole entropy, covering a few main developments since Bekensteins original proposal
62 - G.E. Volovik 2021
We discuss the macroscopic quantum tunneling from the black hole to the white hole of the same mass. Previous calculations in Ref.[1] demonstrated that the probability of the tunneling is $p propto exp(-2S_text{BH})$, where $S_text{BH}$ is the entrop y of the Schwarzschild black hole. This in particular suggests that the entropy of the white hole is with minus sign the entropy of the black hole, $S_text{WH}(M)=- S_text{BH}(M)= - A/(4G)$. Here we use a different way of calculations. We consider three different types of the hole objects: black hole, white hole and the fully static intermediate state. The probability of tunneling transitions between these three states is found using singularities in the coordinate transformations between these objects. The black and white holes are described by the Painleve-Gullstrand coordinates with opposite shift vectors, while the intermediate state is described by the static Schwarzschild coordinates. The singularities in the coordinate transformations lead to the imaginary part in the action, which determines the tunneling exponent. For the white hole the negative entropy is obtained, while the intermediate state -- the fully static hole -- has zero entropy. This procedure is extended to the Reissner-Nordstrom black hole and to its white and static partners, and also to the entropy and temperature of the de Sitter Universe.
The entropy and the attractor equations for static extremal black hole solutions follow from a variational principle based on an entropy function. In the general case such an entropy function can be derived from the reduced action evaluated in a near -horizon geometry. BPS black holes constitute special solutions of this variational principle, but they can also be derived directly from a different entropy function based on supersymmetry enhancement at the horizon. Both functions are consistent with electric/magnetic duality and for BPS black holes their corresponding OSV-type integrals give identical results at the semi-classical level. We clarify the relation between the two entropy functions and the corresponding attractor equations for N=2 supergravity theories with higher-derivative couplings in four space-time dimensions. We discuss how non-holomorphic corrections will modify these entropy functions.
التعليقات
جاري جلب التعليقات جاري جلب التعليقات
سجل دخول لتتمكن من متابعة معايير البحث التي قمت باختيارها
mircosoft-partner

هل ترغب بارسال اشعارات عن اخر التحديثات في شمرا-اكاديميا