A multi-wavelength view of PSR J0437-4715 with NICER and other missions: Radius measurements from far-ultraviolet to hard X-ray pulse profile modeling

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1. Très proche Contexte plus large Pas pertinent

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   Résumé scientifique

   Neutron stars are among the densest objects in the Universe, and mass measurements are crucial to the understanding of their equations of state. Pulsars in tight binaries can be weighed dynamically, but accurate mass estimates are often hampered by uncertainties in orbital inclinations. In this paper, we report on multiepoch optical monitoring of the pulsar binary, PSR J1048+2339, using the 0.5 m RIFT telescope at Lulin Observatory. Our observations reveal frequent optical flares with eclipses caused by the companion. Using the eclipse duration with archival photometric data and orbital ephemeris in the literature, we constrain the inclination to 78.°0±1.°0 and the pulsar mass to 1.79−0.08+0…

2. Très proche Contexte plus large Pas pertinent

   Investigating Dark Matter-Admixed Neutron Stars with NITR Equation of State in Light of PSR J0952-0607

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   Résumé scientifique

   The heaviest pulsar, PSR J0952-0607, with a mass of $M=2.35\pm0.17 \ M_\odot$, has recently been discovered in the disk of the Milky Way Galaxy. In response to this discovery, a new RMF model, "NITR" has been developed. The NITR model's naturalness has been confirmed by assessing its validity for various finite nuclei and nuclear matter (NM) properties, including incompressibility, symmetry energy, and slope parameter values of 225.11, 31.69, and 43.86 MeV, respectively. These values satisfy the empirical/experimental limits currently available. The maximum mass and canonical radius of a neutron star (NS) calculated using the NITR model parameters are 2.35 $M_\odot$ and 12.73 km, respectivel…

3. Proche Contexte plus large Pas pertinent

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   PSR J1907+0602 étudie les impulsions gamma et une nébuleuse de vent de pulsar, sans mesurer la masse ni le rayon de l’étoile.

   Résumé scientifique

   We present multiwavelength studies of the 106.6 ms gamma-ray pulsar PSR J1907+06 near the TeV source MGRO J1908+06. Timing observations with Fermi result in a precise position determination for the pulsar of R.A. = 19h07m547(2), decl. = +06:02:16(2) placing the pulsar firmly within the TeV source extent, suggesting the TeV source is the pulsar wind nebula of PSR J1907+0602. Pulsed gamma-ray emission is clearly visible at energies from 100 MeV to above 10 GeV. The phase-averaged power-law index in the energy range E > 0.1 GeV is = 1.76 \pm 0.05 with an exponential cutoff energy E_{c} = 3.6 \pm 0.5 GeV. We present the energy-dependent gamma-ray pulsed light curve as well as limits on off-pulse…

4. Proche Contexte plus large Pas pertinent

   Ultraslow PSR J0901-4046 with an ultrahigh magnetic field of $3.2\times10^{16}$ G

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   Résumé scientifique

   The recent discovery of a radio-emitting neutron star with an ultralong spin period of 76 s, PSR J0901-4046, raises a fundamental question on how such a slowly rotating magnetized object can be active in the radio band. A canonical magnetic field of $1.3\times10^{14}$ G estimated from the pulsar period and its time derivative is wholly insufficient for PSR J0901-4046 to operate. Consideration of a magnetic inclination angle of $10^\circ$ estimated from the pulse width gives a higher magnetic field of $1.5\times10^{15}$ G, which is still an order of magnitude lower than the necessary minimum of $2.5\times10^{16}$ G following from the death line for radio pulsars with magnetic fields exceeding…

5. Proche Même question Pas pertinent

   Off-Pulse GeV Emission from PSR J0437–4715 and Statistical Properties of Bow-Shock Pulsar Wind Nebulae

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   Off-Pulse GeV Emission analyse les données gamma de PSR J0437−4715, le même pulsar dont l’article modélise les profils thermiques et non thermiques.

   Résumé scientifique

   PSR J0437−4715 is a γ-ray millisecond pulsar, which has been detected by Fermi Large Area Telescope (LAT). To understand the nature, we analyze the GeV γ-ray data obtained with Fermi-LAT around the pulsar region. Based on the pulsar timing ephemeris, we derived the γ-ray pulse profile and defined on-pulse and off-pulse phase intervals. A binned likelihood analysis was performed to investigate the spectral properties of the pulsar across different phase ranges. No spatial extension was detected for off-pulse, with an upper limit radius of 0.12○. The relationship between Lγ and LX is found as $L_{\gamma } \sim L_{X}^{0.6}$. The conversion efficiency from spin-down power to GeV emission of the …

6. Proche Autre approche du problème Pas pertinent

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   Résumé scientifique

   PSR J0835-4510 (a.k.a. the Vela pulsar) is the best studied pulsar in the Southern hemisphere given its high radio brightness and large glitch activity. However, its X-ray brightness is comparatively lower, making the study of its X-ray profile difficult. We aim to investigate the X-ray emission of the Vela pulsar coming from the surface of the neutron star to infer the properties of its hotspots and assess whether they share a common spectral shape. We also aim to prove whether the 2021 glitch affected the hotspots. We used ephemeris obtained from high-cadence radio observations with the radio telescopes of the Argentine Institute of Radio Astronomy to combine all the NICER observations of …

7. Proche Contexte plus large Pas pertinent

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   Résumé scientifique

   HESS J1303$-$631 is an evolved, TeV-bright pulsar wind nebula (PWN) powered by the energetic radio pulsar PSR~J1301$-$6305, offset by $\approx7'$ northwest of the TeV centroid, with an energy-dependent gamma-ray morphology. We present new, deep joint Chandra (108 ks) and XMM-Newton (102 ks) observations of this field. High-resolution Chandra ACIS imaging resolves the pulsar from a neighboring point source that XMM-Newton cannot separate. The pulsar's 2-10 keV spectrum is well described by an absorbed power law with $\Gamma=2.02\pm1.04$ and an unabsorbed luminosity of $3.44\times10^{31}\,{\rm erg\,s^{-1}}$ at $d=4.7$ kpc. Chandra also reveals faint diffuse emission east of the pulsar: a clump…

8. Proche Contexte plus large Pas pertinent

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   PSR J0653+0443 caractérise un système binaire de deux étoiles à neutrons et son orbite excentrique, plutôt que les propriétés de surface d’un pulsar isolé.

   En bref

   La découverte de PSR J0653+0443 révèle un système de deux étoiles à neutrons d’excentricité extrême, éclipsant et source de bouffées périodiques d’ondes gravitationnelles.