Static axisymmetric spacetimes with prescribed multipole moments

Bäckdahl, Thomas; Herberthson, Magnus

doi:10.1088/0264-9381/22/9/009

Cited by 39 publications

(83 citation statements)

References 14 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…It has been shown that the spacetime is uniquely determined by its multipole moments [133][134][135]: in other words, they completely characterize the spacetime geometry outside any stationary body. It has also been shown (in the axisymmetric case) that it is possible to reconstruct the full spacetime from any "well-behaved" set of relativistic multipole moments [136,137].…”

Section: Multipolar Expansions In Newtonian Gravity and In General Rementioning

confidence: 99%

Testing the black hole ‘no-hair’ hypothesis

Cardoso

Gualtieri

2016

Class. Quantum Grav.

222

217

View full text Add to dashboard Cite

Abstract. Black holes in General Relativity are very simple objects. This property, that goes under the name of "no-hair," has been refined in the last few decades and admits several versions. The simplicity of black holes makes them ideal testbeds of fundamental physics and of General Relativity itself. Here we discuss the no-hair property of black holes, how it can be measured in the electromagnetic or gravitational window, and what it can possibly tell us about our universe.

show abstract

Section: Multipolar Expansions In Newtonian Gravity and In General Rementioning

confidence: 99%

Testing the black hole ‘no-hair’ hypothesis

Cardoso

Gualtieri

2016

Class. Quantum Grav.

222

217

View full text Add to dashboard Cite

show abstract

“…the Quadrupole Solution itself, and more recently in [11], [12] a method has been proposed for obtaining the general terms of the series (the coefficients a n ) that define the Pure 2 N -pole Solutions. In fact, the general term of the series corresponding to the gravitational Dipole and the solutions with Monopole plus any other 2 N -pole moment are written specifically.…”

Section: Calculation Of Msa Coordinates For Any Multipole Solutionmentioning

confidence: 99%

“…Moreover, the Weyl family of solutions depends on arbitrary constants, a n , in principle without any physical criteria to choose one or another solution from them, whereas the function u would allow us to deal, in a very simple form, with the Relativistic Multipole Solutions. This has been the aim of some authors and their works devoted to obtain solutions of the Einstein vacuum equations with a finite number of prescribed RMM [7,9,11,12].…”

Section: Introductionmentioning

confidence: 99%

On the calculation and interpretation of MSA coordinates

Hernández‐Pastora¹

2010

Class. Quantum Grav.

View full text Add to dashboard Cite

The static solutions of the axially symmetric vacuum Einstein equations with a finite number of Relativistic Multipole Moments (RMM) are described by means of a function that can be written in the same analytic form as the Newtonian gravitational multipole potential. A family of so-called MSA (Multipole-Symmetry Adapted) coordinates are introduced to perform the transformation of the Weyl solutions; a procedure for their calculation at any multipole order is given, and the results for a low order are shown.In analogy with a previous result [10] obtained in Newtonian gravity, the existence of a symmetry of a certain system of differential equations leading to the determination of that kind of multipole solutions in General Relativity is explored. The relationship between the existence of this kind of coordinates and the symmetries mentioned is proved for some cases, and the characterization of the MSA system of coordinates by means of this relationship is discussed.

show abstract

“…The stellar shape affects the gravitational field outside the source, which controls various NS observables. The exterior gravitational field can be described through a multipolar decomposition (Backdahl & Herberthson 2005;Backdahl 2007), just as when describing the exterior electromagnetic field of a charged object with multipole moments.…”

Section: Introductionmentioning

confidence: 99%

Three-Hair Relations for Rotating Stars: Nonrelativistic Limit

Stein

Yagi

Yunes

2014

ApJ

172

View full text Add to dashboard Cite

The gravitational field outside of astrophysical black holes is completely described by their mass and spin frequency, as expressed by the no-hair theorems. These theorems assume vacuum spacetimes, and thus they apply only to black holes and not to stars. Despite this, we analytically find that the gravitational potential of arbitrarily rapid rigidly rotating stars can still be described completely by only their mass, spin angular momentum, and quadrupole moment. Although these results are obtained in the nonrelativistic limit (to leading order in a weak-field expansion of general relativity, GR), they are also consistent with fully relativistic numerical calculations of rotating neutron stars. This description of the gravitational potential outside the source in terms of just three quantities is approximately universal (independent of equation of state). Such universality may be used to break degeneracies in pulsar and future gravitational wave observations to extract more physics and test GR in the strong-field regime.

show abstract

Static axisymmetric spacetimes with prescribed multipole moments

Cited by 39 publications

References 14 publications

Testing the black hole ‘no-hair’ hypothesis

Testing the black hole ‘no-hair’ hypothesis

On the calculation and interpretation of MSA coordinates

Three-Hair Relations for Rotating Stars: Nonrelativistic Limit

Contact Info

Product

Resources

About