A Study of the Pulsed Radio Emission from XTE J1810−197

Hotan, A. W.; Long, S. R.; Dickey, John M.; Dolley, T. J.

doi:10.1086/520796

Cited by 3 publications

(3 citation statements)

References 23 publications

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“…Middle panel: flux density and its variability as measured at various frequencies as a function of time. We also added data measured by Hotan et al (2007) at 1.4 and 4.8 GHz (shown as crosses and stars, respectively) and Camilo et al (2007c) at 1.42 and 4.8 GHz (shown as bars and exes, respectively). Bottom panel: derived spectral indices of the MP as a function of time.…”

Section: Data Analysis and Resultsmentioning

confidence: 99%

“…The nominal conservative uncertainties for our flux density measurements are about 10 per cent (see also ). In addition to our flux densities, we also utilize published flux densities measured at 1.42 and 4.8 GHz with the Very Large Array (VLA; Camilo et al 2007c) and at 1.4 and 4.8 GHz at the Mount Pleasant observatory (Hotan et al 2007) (see Fig. 3).…”

Section: Data Analysis and Resultsmentioning

confidence: 99%

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Radio spectrum of the AXP J1810−197 and of its profile components

Lazaridis¹,

Jessner²,

Krämer³

et al. 2008

Monthly Notices of the Royal Astronomical Society

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As part of a European Pulsar Network (EPN) multitelescope observing campaign, we performed simultaneous multifrequency observations at 1.4, 4.9 and 8.4 GHz during 2006 July and quasi‐simultaneous multifrequency observations from 2006 December until 2007 July at 2.7, 4.9, 8.4, 14.6 and 32 GHz, in order to obtain flux density measurements and spectral features of the 5.5 s radio‐emitting magnetar AXP J1810−197. We monitored the spectral evolution of its pulse shape which consists of a main pulse (MP) and an interpulse (IP). We present the flux density spectrum of the average profile and of the separate pulse components of this first‐known radio‐emitting transient anomalous X‐ray pulsar. We observe a decrease in the flux density by a factor of 10 within 8 m and follow the disappearance of one of the two main components. Although the spectrum is generally flat, we observe large fluctuations of the spectral index with time. For that reason, we have made some measurements of modulation indices for individual pulses in order to investigate the origin of these fluctuations.

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Section: Data Analysis and Resultsmentioning

confidence: 99%

Section: Data Analysis and Resultsmentioning

confidence: 99%

Radio spectrum of the AXP J1810−197 and of its profile components

Lazaridis¹,

Jessner²,

Krämer³

et al. 2008

Monthly Notices of the Royal Astronomical Society

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“…The polarization data presented here do not strengthen or weaken this scenario, but points towards an observational test. As XTE 1810−197 is gradually returning to quiescence, it will be as interesting to look for orthogonal PA jumps and a decrease in the linear polarization as for intermittent emission typical of RRATs (tentative evidence of the latter can be found in observations in Hotan et al 2007).…”

Section: Discussionmentioning

confidence: 99%

Radio polarization measurements from RRAT J1819−1458

Karastergiou

Hotan

Straten

et al. 2009

Monthly Notices of the Royal Astronomical Society: Letters

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We present the first polarization measurements of the radio emission from RRAT J1819−1458. Our observations, conducted in parallel to regular timing sessions, have yielded a small number of bright and polarized pulses. The polarization characteristics and integrated profile resemble those of normal pulsars with average spin‐down energy : moderate to low linear polarization in the integrated profile despite relatively high polarization in the individual pulses. On average, a small degree of circular polarization is also observed. The polarization position angle (PA) executes a remarkably smooth, steep S‐shaped curve, interrupted by two orthogonal jumps. Based on the shape of the PA swing, we place some constraints on the emission geometry. We compare these polarization properties to those of other radio‐emitting neutron star populations, including young pulsars, pulsars with a high surface magnetic field and radio‐emitting magnetars. From the polarization measurements, the Faraday rotation measure of this rotating radio transient is derived.

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Pulse frequency fluctuations of magnetars

Cerri-Serim

Serim

Şahiner

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Using RXTE, Chandra, XMM-Newton and Swift observations, we for the first time construct the power spectra and torque noise strengths of magnetars.For some of the sources, we measure strong red noise on timescales months to years which might be a consequence of their outbursts. We compare noise strengths of magnetars with those of radio pulsars by investigating possible correlations of noise strengths with spin-down rate, magnetic field and age.Using these correlations, we find that magnetar noise strengths are obeying similar trends with radio pulsars. On the contrary, we do not find any correlation between noise strength and X-ray luminosity which was seen in accretion powered pulsars. Our findings suggest that the noise behaviour of magnetars resembles that of radio pulsars but they possess higher noise levels likely due to their stronger magnetic fields.

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A Study of the Pulsed Radio Emission from XTE J1810−197

Cited by 3 publications

References 23 publications

Radio spectrum of the AXP J1810−197 and of its profile components

Radio spectrum of the AXP J1810−197 and of its profile components

Radio polarization measurements from RRAT J1819−1458

Pulse frequency fluctuations of magnetars

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