Equimolecular Mixture of Calamitic and Bent-Core Thiobenzoates

Chruściel, J.; Wantusiak, B.; Ossowska‐Chruściel, M. D.

doi:10.12693/aphyspola.122.375

Cited by 12 publications

(16 citation statements)

References 14 publications

(13 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Since the entropy of any black hole is proportional to the area A of horizon cross-sections, we see that the orbiting moon does not affect the entropy of the companion hole. (The result (23) holds for any cross-section H , a fact that can be seen a priori from the helical symmetry of the perturbed spacetime. )…”

Section: Perturbations In Horizon Surface Area Angular Velocity and S...mentioning

confidence: 77%

“…We will show that these properties imply the vanishing of the expansion and shear of the geodesic generators of the perturbed event horizon. By rigidity arguments [2,[22][23][24][25][26] this should in turn imply that the perturbed horizon is a Killing horizon. 3 The perturbed horizon then has a well-defined surface gravity and angular frequency, and we are able to compute these quantities (along with the perturbed surface area) without further assumptions about the spacetime.…”

Section: Spacetime Of a Black Hole With Moonmentioning

confidence: 99%

“…We also obtain formulas for the changes in horizon area and angular velocity, Eqs. (23) and (25) below. While the area perturbation vanishes, the rotation frequency perturbation is positive (see Fig.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Thermodynamics of a black hole with moon

Gralla

Tiec

2013

Phys. Rev. D

View full text Add to dashboard Cite

For a Kerr black hole perturbed by a particle on the "corotating" circular orbit (angular velocity equal to that of the unperturbed event horizon), the black hole remains in equilibrium in the sense that the perturbed event horizon is a Killing horizon of the helical Killing field. The associated surface gravity is constant over the horizon and should correspond to the physical Hawking temperature. We calculate the perturbation in surface gravity/temperature, finding it negative: the moon has a cooling effect on the black hole. We also compute the change in horizon angular frequency, which is positive, and the change in surface area/entropy, which vanishes.

show abstract

Section: Perturbations In Horizon Surface Area Angular Velocity and S...mentioning

confidence: 77%

Section: Spacetime Of a Black Hole With Moonmentioning

confidence: 99%

See 1 more Smart Citation

Thermodynamics of a black hole with moon

Gralla

Tiec

2013

Phys. Rev. D

View full text Add to dashboard Cite

show abstract

“…This requirement is satisfied in particular by non-degenerate Killing horizons in the static vacuum spacetime [34]. The listed data representing a non-rotating horizon 12 uniquely determines then the metric and Maxwell field of a static spacetime in the connected region in which the Killing field is timelike.…”

Section: B Necessary Conditions: Data At △ and The Metric Expansionmentioning

confidence: 99%

Neighborhoods of isolated horizons and their stationarity

Lewandowski

Pawłowski

2014

Class. Quantum Grav.

View full text Add to dashboard Cite

A distinguished (invariant) Bondi-like coordinate system is defined in the spacetime neighbourhood of a non-expanding horizon of arbitrary dimension via geometry invariants of the horizon. With its use, the radial expansion of a spacetime metric about the horizon is provided and the free data needed to specify it up to given order are determined in spacetime dimension 4. For the case of an electro-vacuum horizon in 4-dimensional spacetime the necessary and sufficient conditions for the existence of a Killing field at its neighbourhood are identified as differential conditions on the horizon data and data on null surface transversal to the horizon.PACS numbers: 04.70.Bw, 04.50.Gh I. INTRODUCTIONSystematic studies of black holes in various approaches to quantum gravity as well as accurate description of the dynamical evolution of these exotic objects require a quasi-local description formalism -where a black hole can be treated as "object in the lab" and the global spacetime structure of the universe far away from it can be neglected. Among several approaches to construct such formalism [1, 2] one of considerable success is the theory of Isolated Horizons [3][4][5]. This approach was originally inspired by ideas of Pejerski and Newman [1], next shaped into a solid formalism by Ashtekar [6] and subsequently developed by many researchers. Its main feature is the representation of a black hole in equilibrium through its surface -the non-expanding (or isolated) horizon -a null cylinder of codimension 1 and of compact spatial slices embedded in a Lorentzian spacetime. The black hole is characterized by the geometry (and possibly matter fields) data on this surface only. Both geometry aspects [6,7] and the mechanics [8,9] have been systematically studied in spacetime dimension 4 and then extended to general dimension [10][11][12], the latter including in particular asymptotically Anti-deSitter spacetimes [13]. Also various matter content at the horizon has been considered [14] as well as the properties of symmetric horizons [15] and their relation with standard black hole solutions [16,17]. The formalism has been further extended to the non-equilibrium situations through the Dynamical Horizons [18] (see also [4]). It is vastly applied in numerical relativity (see for example [19]) as well as in black hole description in loop quantum gravity [20] -especially as the basis for entropy calculations (see for example [21]). The extension to this formalism has found applications also in supergravity [22] and string theory inspired gravity [23].The quasi-locality of the theory is a great advantage, as only the geometry objects at the horizon are relevant in the description, however for this very reason one misses the information about the black hole neighbourhood. However, the success of the formalism of near horizon geometries [24] shows clearly, that there is a strong demand for any black hole description method to be able to also "handle" its neighbourhood, a feature particularly relevant for the studies of black hole spaceti...

show abstract

“…But these works considered only the Einstein equations without cosmological constant. Few works including [30][31][32][33][34] investigated the cosmological constant issue. Their results imply that the geometric behavior for spacetimes with vanishing cosmological constant Λ is much different to the behavior for spacetimes with non-vanishing Λ no matter how small Λ is.…”

Section: Introductionmentioning

confidence: 99%

Note on the gravitational and electromagnetic radiation for the Einstein-Maxwell equations with cosmological constant

He,

Cao,

Jing

2017

Preprint

View full text Add to dashboard Cite

In the middle of last century, Bondi and his coworkers proposed an out going boundary condition for the Einstein equations. Based on such boundary condition the authors theoretically solved the puzzle of the existence problem of gravitational wave. Currently many works on gravitational wave source modeling use Bondi's result to do the analysis including the gravitational wave calculation in numerical relativity. Recently more and more observations imply that the Einstein equations should be modified with an nonzero cosmological constant. In this work we use Bondi's original method to treat the Einstein equations with cosmological constant for theoretical curiosity. We find that the gravitational wave does not essentially exist if Bondi's original out going boundary condition is imposed. We find this unphysical result is due to the non-consistency between Bondi's original out going boundary condition and the Einstein equations with cosmological constant. Based on theoretical analysis, we propose an new Bondi-type out going boundary condition for the Einstein equations with cosmological constant. With this new boundary condition, the gravitational wave behavior for the Einstein equations with cosmological constant is similar to the Einstein equations without cosmological constant. In particular, when the cosmological constant goes to zero, the behavior of the Einstein equations without cosmological constant is recovered. Together with gravitational wave, electromagnetic wave is also analyzed. The boundary conditions for electromagnetic wave does not depend on the cosmological constant.

show abstract

Equimolecular Mixture of Calamitic and Bent-Core Thiobenzoates

Cited by 12 publications

References 14 publications

Thermodynamics of a black hole with moon

Thermodynamics of a black hole with moon

Neighborhoods of isolated horizons and their stationarity

Note on the gravitational and electromagnetic radiation for the Einstein-Maxwell equations with cosmological constant

Contact Info

Product

Resources

About