Zobrazeno 1 - 10
of 62
pro vyhledávání: '"Espinoza, Cristobal"'
Autor:
Espinoza, Cristóbal M., Kuiper, Lucien, Ho, Wynn C. G., Antonopoulou, Danai, Arzoumanian, Zaven, Harding, Alice K., Ray, Paul S., Younes, George
The way pulsars spin down is not understood in detail, but a number of possible physical mechanisms produce a spin-down rate that scales as a power of the rotation rate ($\dot\nu\propto-\nu^n$), with the power-law index $n$ called the braking index.
Externí odkaz:
http://arxiv.org/abs/2409.10759
Autor:
Hu, Chin-Ping, Kuiper, Lucien, Harding, Alice K., Younes, George, Blumer, Harsha, Ho, Wynn C. G., Enoto, Teruaki, Espinoza, Cristobal M., Gendreau, Keith
We report on our monitoring of the strong-field magnetar-like pulsar PSR J1846-0258 with the Neutron Star Interior Composition Explorer (NICER) and the timing and spectral evolution during its outburst in August 2020. Phase-coherent timing solutions
Externí odkaz:
http://arxiv.org/abs/2306.00902
Autor:
Ho, Wynn C. G., Kuiper, Lucien, Espinoza, Cristobal M., Guillot, Sebastien, Ray, Paul S., Smith, D. A., Bogdanov, Slavko, Antonopoulou, Danai, Arzoumanian, Zaven, Bejger, Michal, Enoto, Teruaki, Esposito, Paolo, Harding, Alice K., Haskell, Brynmor, Lewandowska, Natalia, Maitra, Chandreyee, Vasilopoulos, Georgios
Publikováno v:
Astrophys. J. 939, 7 (2022)
Measuring a pulsar's rotational evolution is crucial to understanding the nature of the pulsar. Here we provide updated timing models for the rotational evolution of six pulsars, five of which are rotation phase-connected using primarily NICER X-ray
Externí odkaz:
http://arxiv.org/abs/2205.02865
The Earth's magnetosphere represents a natural plasma laboratory that allows us to study the behavior of particle distribution functions in the absence of Coulomb collisions, typically described by the Kappa distributions. We have investigated the pr
Externí odkaz:
http://arxiv.org/abs/2101.07305
Autor:
Ho, Wynn C. G., Espinoza, Cristobal M., Arzoumanian, Zaven, Enoto, Teruaki, Tamba, Tsubasa, Antonopoulou, Danai, Bejger, Michal, Guillot, Sebastien, Haskell, Brynmor, Ray, Paul S.
Publikováno v:
Mon. Not. R. Astron. Soc. 498, 4605-4614 (2020)
PSR J0537-6910, also known as the Big Glitcher, is the most prolific glitching pulsar known, and its spin-induced pulsations are only detectable in X-ray. We present results from analysis of 2.7 years of NICER timing observations, from 2017 August to
Externí odkaz:
http://arxiv.org/abs/2009.00030
Autor:
Ho, Wynn C. G., Guillot, Sebastien, Parkinson, P. M. Saz, Limyansky, B., Ng, C. -Y., Bejger, Michal, Espinoza, Cristobal M., Haskell, B., Jaisawal, Gaurava K., Malacaria, C.
Publikováno v:
Mon. Not. R. Astron. Soc. 498, 4396-4403 (2020)
PSR J1813-1749 is one of the most energetic rotation-powered pulsars known, producing a pulsar wind nebula (PWN) and gamma-ray and TeV emission, but whose spin period is only measurable in X-ray. We present analysis of two Chandra datasets that are s
Externí odkaz:
http://arxiv.org/abs/2009.00031
Publikováno v:
Phys. Rev. D 101, 103009 (2020)
During their most recent observing run, LIGO/Virgo reported the gravitational wave (GW) transient S191110af, a burst signal at a frequency of 1.78 kHz that lasted for 0.104 s. While this signal was later deemed non-astrophysical, genuine detections o
Externí odkaz:
http://arxiv.org/abs/2003.12082
Autor:
Espinoza, Cristóbal M.
Braking indices are used to describe the evolution of pulsars rotation, and can offer insights into the braking mechanism that dominates the slow down. Here we discuss the main difficulties associated with measuring braking indices and the complexity
Externí odkaz:
http://arxiv.org/abs/1711.01916
Pulsars are rotating neutron stars that are renowned for their timing precision, although glitches can interrupt the regular timing behavior when these stars are young. Glitches are thought to be caused by interactions between normal and superfluid m
Externí odkaz:
http://arxiv.org/abs/1703.00932
Publikováno v:
Science Adv. 1, e1500578 (2015)
Pulsars are known for their superb timing precision, although glitches can interrupt the regular timing behavior when the stars are young. These glitches are thought to be caused by interactions between normal and superfluid matter in the crust of th
Externí odkaz:
http://arxiv.org/abs/1510.00395