Perturbative approach to the structure of rapidly rotating neutron stars

Benhar, Omar; Ferrari, Valeria; Gualtieri, Leonardo; Marassi, Stefania

doi:10.1103/physrevd.72.044028

Cited by 118 publications

(246 citation statements)

References 30 publications

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“…Fig. 5 in Benhar et al 2005). We have also given estimates of the magnetic field induced by rotation of the interior charge distribution in neutron stars satisfying the condition of global, but not local, charge neutrality.…”

Section: Discussionmentioning

confidence: 99%

“…However, the latter effect is negligible for this specific case (P ≈ 4.3 s), see for instance Fig. 5 in (Benhar et al 2005), where no deviations of I from its spherical value appear for such long rotation periods.…”

Section: Inference Of Pulsar's Propertiesmentioning

confidence: 99%

“…1, which practically overlaps the non-rotating mass-radius relation. The accuracy of the approximation increases for stiffer EOS (see Benhar et al 2005, for details), as the ones given by σ-ω-ρ relativistic nuclear mean field models.…”

Section: Neutron Star Structurementioning

confidence: 99%

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On the Magnetic Field of Pulsars With Realistic Neutron Star Configurations

Belvedere

Rueda

Ruffini

2015

ApJ

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We have recently developed a neutron star model fulfilling global and not local charge neutrality, both in the static and in the uniformly rotating cases. The model is described by the coupled Einstein-Maxwell-ThomasFermi (EMTF) equations, in which all fundamental interactions are accounted for in the framework of general relativity and relativistic mean field theory. Uniform rotation is introduced following the Hartle's formalism. We show that the use of realistic parameters of rotating neutron stars obtained from numerical integration of the self-consistent axisymmetric general relativistic equations of equilibrium leads to values of the magnetic field and radiation efficiency of pulsars very different from estimates based on fiducial parameters assuming a neutron star mass, M = 1.4 M ⊙ , radius R = 10 km, and moment of inertia, I = 10 45 g cm 2 . In addition, we compare and contrast the magnetic field inferred from the traditional Newtonian rotating magnetic dipole model with respect to the one obtained from its general relativistic analog which takes into due account the effect of the finite size of the source. We apply these considerations to the specific high-magnetic field pulsars class and show that, indeed, all these sources can be described as canonical pulsars driven by the rotational energy of the neutron star, and with magnetic fields lower than the quantum critical field for any value of the neutron star mass.

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Section: Discussionmentioning

confidence: 99%

Section: Inference Of Pulsar's Propertiesmentioning

confidence: 99%

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On the Magnetic Field of Pulsars With Realistic Neutron Star Configurations

Belvedere

Rueda

Ruffini

2015

ApJ

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“…However, to understand nuclear effects correctly, recently developed models for CCQE interactions (for example [41][42][43][44][45]) are more promising. To tune these models, we need to compare with CCQE cross section data.…”

Section: Ccqe Cross Section Measurementmentioning

confidence: 99%

A Measurement of the muon neutrino charged current quasielastic interaction and a test of Lorentz violation with the MiniBooNE experiment

Katori

2008

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school was successful since I relied 100% on your support. For FINeSSE, you taught me everything step by step because I didn't know anything. For Lorentz violation, even though it was a spin-off subject for me and you, but you were so generous, supportive, and patient.And for MiniBooNE, the CCQE work couldn't have been done without your ideas. I am really proud of the amount of work I present in this thesis; it is the evidence of what a good work relationship we have. Finally I want to apologize for my bad English and for how you always had to correct it, including in this thesis. This acknowledgments section is the only one place in all my writings for which you didn't correct my English! Thank you Rex.My first three years were supported by the people in Indiana.I wish to give sincere appreciation to Chris Cox and Nikodem Pop lawski, I think it was my fate to see you from the very first day in US. I had a hard time (as you know), but because of your help, I not only survived, but also changed my style to be more suitable in this country. No one ever was so influential for me as Chris, I think. And Niko, before Thank you for sharing good times with me. I also want to thank Hans-Otto Mayer, Jack Doskow, and Gerard Visser for your help and inspiration for the work on FINeSSE. Thank you everyone.My friends from the classroom, it is a very strange feeling that now all we are going somewhere to do something, but we have known each other more than six years! Liliana Cabellero, you changed shy Teppei...to an emotional salsa dancer! If the dancing is my mother of energy, then Lily is founding mother of energetic Teppei. Muchas gracias. Leah Welty and Jason Rieger are the first real American students I met. When you described Chicago, I didn't understand very much, but now, yeah, I love this city and want to stay here more. Heechang Na, thank you for talking with me every time I stopped by your office, v because you are so kind and welcome and easy to talk with! Haiyang "Ocean" Yan, I am proud that I nicknamed you. I think you are a very good physicist. Thank you for teaching me a lot about Chinese history and physics. I always enjoyed it. Masaki (& Shizuka) Ishitsuka is the first Japanese fellow I met at Indiana even though I left Bloomington before you came. I always enjoyed talking about neutrinos with you, your view of physics is very unique and interesting to me. Thank you. Yun-Chan, Tony, George, Jay, Helber, Jorge, Shinya... I had so much fun in Indiana because of you. Thank you very much.One of the reasons I wanted to be a physicist is that physicists make friends all over the world so easily. I met many friends at conferences, summer schools, etc. Thank you to everyone who called me a crazy Japanese, even uploading my stupidities on YouTube.

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“…Calculations of the frequency and damping time of the fundamental quadrupole mode for various models of the equation of state, such as those in [35,36], indicate that the frequency lies in the range 1 ν 0 3 kHz and the damping time lies in the range 0.05 τ 0 0.5 seconds.…”

Section: Pulsar Glitches and Gravitational Radiationmentioning

confidence: 99%

Search for gravitational waves associated with the August 2006 timing glitch of the Vela pulsar

Abadie¹,

Abbott²,

Abbott³

et al. 2011

Phys. Rev. D

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The physical mechanisms responsible for pulsar timing glitches are thought to excite quasinormal mode oscillations in their parent neutron star that couple to gravitational-wave emission. In August 2006, a timing glitch was observed in the radio emission of PSR B0833-45, the Vela pulsar. At the time of the glitch, the two colocated Hanford gravitational-wave detectors of the Laser Interferometer Gravitational-wave observatory (LIGO) were operational and taking data as part of the fifth LIGO science run (S5). We present the first direct search for the gravitational-wave emission associated with oscillations of the fundamental quadrupole mode excited by a pulsar timing glitch. No gravitational-wave detection candidate was found. We place Bayesian 90% confidence upper limits of 6.3 x 10(-21) to 1.4 x 10(-20) on the peak intrinsic strain amplitude of gravitational-wave ring-down signals, depending on which spherical harmonic mode is excited. The corresponding range of energy upper limits is 5.0 x 10(44) to 1.3 x 10(45) erg

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Perturbative approach to the structure of rapidly rotating neutron stars

Cited by 118 publications

References 30 publications

On the Magnetic Field of Pulsars With Realistic Neutron Star Configurations

On the Magnetic Field of Pulsars With Realistic Neutron Star Configurations

A Measurement of the muon neutrino charged current quasielastic interaction and a test of Lorentz violation with the MiniBooNE experiment

Search for gravitational waves associated with the August 2006 timing glitch of the Vela pulsar

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