Investigations of the emission geometry of the four-component radio pulsar J0631+1036

Teixeira, Mateus M.; Rankin, Joanna M.; Wright, Geoffrey; Dyks, J.

doi:10.1093/mnras/stv2520

Cited by 6 publications

(3 citation statements)

References 20 publications

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“…The near even spacing of its four features, the deep emission minimum in the profile center and the weakness of its outer pair with respect to the inner pair distinguish its unusual profile from the rest of the four-component population. Teixeira et al (2016) show that such a profile can be explained by the widely used core-double-cone beaming model but needs an unrealistic fine tuning when assuming circular beams.…”

Section: 1mentioning

confidence: 98%

Revealing the Most Energetic Light from Pulsars and Their Nebulae

Fidalgo

2019

Springer Theses

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© David Carreto Fidalgo, 2018 157 8.1 The young and energetic gamma-ray pulsar psr j0631+1036 158 8.2 Observational hints of a TeV pulsar wind nebula 161 9 MAGIC observations of PSR J0631: analysis and results 165 9.1 Data set and quality selection 166 9.2 Moonlight data and extended source analysis 168 9.3 Analysis results and discussion 172 Summary and conclusions 177 Appendix 183 A Interaction processes in very-high-energy astrophysics 185 B Pulsar timing 191 C The on-site analysis chain of MAGIC 195 D Details on the Crab pulsar analysis 201 References 207 viii Thesis advisor: Abstract Background. The observation of Very-High-Energy (vhe, >100 GeV) gamma raysis key in studying the non-thermal sources of radiation in our Universe. Pulsars and Pulsar Wind Nebulae (pwne) are two source classes that are known to emit vhe gamma rays. While pulsar wind nebulae are the dominant vhe gamma-ray source class in our galaxy, only two pulsars have been detected above 100 GeV so far. Most pulsar models explain gamma-ray emission via synchro-curvature radiation in the radiation-reaction limited regime, which leads to a sharp cut-off in the pulsar spectrum at energies of a few GeV.However, the detection of pulsed emission from the Crab pulsar up to hundreds of GeV by magic and veritas, suggests that classical pulsar models do not provide a full picture of the emission mechanisms at work. TeV pulsar wind nebulae, on the other hand, are observed via their inverse Compton radiation and are primarily found around young and energetic pulsars located towards the inner Milky Way. Detections of TeV pwne in the outer part of our galaxy are scarce, but could provide valuable input for the connection between the interstellar radiation field and the pwn luminosity.Aims. The principle goal of this thesis is to study the very-high-energy emission of the Crab pulsar. We aim to answer the long-standing question up to what energies pulsars are able to radiate and what is the emission mechanism behind it. We further exploit the pulsed vhe emission from the Crab to investigate fundamental physics testing for Lorentz Invariance Violation (liv), in terms of a wavelength dependent speed of light. To deepen our understanding of the pulsar emission mechanism at the highest energies, further pulsars have to be discovered above 100 GeV. To this end we search among pulsars already detected at around 1 GeV for the best candidates to emit gamma-rays in the vhe range.Another aim of this thesis is to discover a new pulsar wind nebula towards the outer part of our galaxy with the magic telescopes.ix Thesis advisor:Methods. We analyzed more than 400 hours of good-quality data of the Crab pulsar obtained by the magic telescopes between 2007 and 2016. This unprecedented large data set allowed us to effectively explore the Crab pulse profile and spectrum above 400 GeV.To test for Lorentz invariance violation, primarily foreseen by theories of quantum gravity, we modeled the vhe emission of the Crab pulsar and employed Bayesian inference to derive lower limits on...

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Section: 1mentioning

confidence: 98%

Revealing the Most Energetic Light from Pulsars and Their Nebulae

Fidalgo

2019

Springer Theses

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“…J0631+1036: This pulsar presents a rare example of a fourcomponent pulsar. Teixeira et al (2016) studied the pulsar and worked out the geometry that we use here to model its profiles. The authors outline issues with accommodating the inner cone, but the dimension do satisfy the double cone model.…”

Section: B0540+23mentioning

confidence: 99%

Pulsar emission beam geometry of radio broad-band Arecibo sources

Olszanski

Rankin

Venkataraman

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present radio pulsar emission beam analyses and models with the primary intent of examining pulsar beam geometry and physics over the broadest band of radio frequencies reasonably obtainable. We consider a set of well-studied pulsars that lie within the Arecibo sky. These pulsars stand out for the broad frequency range over which emission is detectable, and have been extensively observed at frequencies up to 4.5 GHz and down to below 100 MHz. We utilize published profiles to quantify a more complete picture of the frequency evolution of these pulsars using the core/double-cone emission beam model as our classification framework. For the low-frequency observations, we take into account measured scattering time-scales to infer intrinsic versus scatter broadening of the pulse profile. Lastly, we discuss the populational trends of the core/conal class profiles with respect to intrinsic parameters. We demonstrate that for this sub-population of pulsars, core and conal dominated profiles cluster together into two roughly segregated $P - \dot{P}$ populations, lending credence to the proposal that an evolution in the pair-formation geometries is responsible for core/conal emission and other emission effects such as nulling and mode-changing.

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“…The debate between the "corecone" beam models and other models (such as the "patchy" beam, fan-beam, microbeam pattern et al) as well as multi-frequency observed data have been persisted by many authors (e.g. Lyne & Manchester 1988;Kramer et al 1994;Manchester 1995;Gil & Krawczyk 1996;Melrose 1999;Mitra & Deshpande 1999;Gangadhara et al 2001;Han & Manchester 2001;Kijak & Gil 2002;Manchester et al 2005;Karastergiou & Johnston 2007;Maciesiak et al 2012;Beskin & Philippov 2012;Fonseca et al 2014;Wang et al 2014;Cerutti et al 2016;Dyks et al 2016;Pierbattista et al 2016;Teixeira et al 2016). Besides, some theoretical perspectives (such as: the radio radiation beam is a hollow beam without a core cone; the pulse profiles at lower frequency are wider than those at higher frequencies) have been challenged by a large number of observations.…”

Section: Introductionmentioning

confidence: 99%

Investigating the multifrequency pulse profiles of PSRs B0329+54 and B1642–03 in an inverse Compton scattering model

Shang

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The emission geometries, e.g. the emission region height, the beam shape, and radiusto-frequency mapping, are important predictions of pulsar radiation model. The multiband radio observations carry such valuable information. In this paper, we study two bright pulsars, (PSRs B0329+54 and B1642−03) and observe them in high frequency (2.5 GHz, 5 GHz, and 8 GHz). The newly acquired data together with historical archive provide an atlas of multi-frequency profiles spanning from 100 MHz to 10 GHz. We study the frequency evolution of pulse profiles and the radiation regions with the these data. We firstly fit the pulse profiles with Gaussian functions to determine the phase of each component, and then calculate the radiation altitudes of different emission components and the radiation regions. We find that the inverse Compton scattering (ICS) model can reproduce the radiation geometry of these two pulsars. But for PSR B0329+54 the radiation can be generated in either annular gap (AG) or core gap (CG), while the radiation of PSR B1642−03 can only be generated in the CG. This difference is caused by the inclination angle and the impact angle of these two pulsars. The relation of beaming angle (the angle between the radiation direction and the magnetic axis) and the radiation altitudes versus frequency is also presented by modelling the beam-frequency evolution in the ICS model. The multi-band pulse profiles of these two pulsars can be described well by the ICS model combined with the CG and AG.

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Investigations of the emission geometry of the four-component radio pulsar J0631+1036

Cited by 6 publications

References 20 publications

Revealing the Most Energetic Light from Pulsars and Their Nebulae

Revealing the Most Energetic Light from Pulsars and Their Nebulae

Pulsar emission beam geometry of radio broad-band Arecibo sources

Investigating the multifrequency pulse profiles of PSRs B0329+54 and B1642–03 in an inverse Compton scattering model

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