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Journal articles on the topic 'Pulsar polarimetry'

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Author: Grafiati

Published: 4 June 2021

Last updated: 11 February 2022

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1

Tremblay, Steven E., Mengyao Xue, N. D. Ramesh Bhat, and Caterina Tiburzi. "Verifying the low frequency pulsar polarimetry of the MWA." Proceedings of the International Astronomical Union 13, S337 (September 2017): 416–17. http://dx.doi.org/10.1017/s174392131701033x.

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AbstractStudying the polarised properties of pulsars has a rich history giving unique geometric information about pulsars as well as testing the theories of pulsar emission physics. Performing such studies with the MWA has the attraction that the percentage of linear polarisation of many pulsars increases as the observing frequency decreases. Here we discuss the strategies being employed to verify the polarimetric response of the MWA’s high time resolution data.

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2

Shearer, Andrew, and Eoin O’ Connor. "Optical pulsars and polarimetry." Proceedings of the International Astronomical Union 13, S337 (September 2017): 191–94. http://dx.doi.org/10.1017/s174392131700998x.

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AbstractDespite the early optical detection of the Crab pulsar in 1969, optical pulsars have become the poor cousin of the neutron star family. Only five normal pulsars have been observed to pulse in the optical waveband. A further three magnetars/SGRs have been detected in the optical/near IR. Optical pulsars are intrinsically faint with a first order luminosity, predicted by Pacini, to be proportional to P−10, where P is the pulsar’s period. Consequently they require both large telescopes, generally over-subscribed, and long exposure times, generally difficult to get. However optical observations have the benefit that polarisation and spectral observations are possible compared to X-ray and gamma-ray observations where polarisation measurements are limited. Over the next decade the number of optical pulsars should increase as optical detectors approach 100% quantum efficiency and as we move into the era of extremely large telescopes where limiting fluxes will be 30 to 100 times fainter compared to existing optical telescopes.

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3

von Hoensbroech, A., and K. M. Xilouris. "Effelsberg multifrequency pulsar polarimetry." Astronomy and Astrophysics Supplement Series 126, no. 1 (November 1997): 121–49. http://dx.doi.org/10.1051/aas:1997255.

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4

Hoensbroech, Alexis von. "Pulsar Polarimetry – New Aspects at High Radio Frequencies." International Astronomical Union Colloquium 177 (2000): 267–68. http://dx.doi.org/10.1017/s0252921100059674.

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AbstractPulsar polarimetry is an important tool for the investigation of the physical processes and the environment in the magnetosphere. However, the great variety of observed polarization states and the few obvious systematics hamper a straightforward interpretation. In this paper it is shown that the polarimetric features of pulsars are much more systematic at high radio frequencies. An analysis of 116 profiles at 4.85 GHz reveals a clear correlation between the degree of polarization andĖ. Also evidence is shown for pulsars with a heavily increasing degree of circular polarization. Further, a basic concept of a simple magnetospheric propagation scenario is presented, which can account for a variety of polarimetric properties of pulsars.

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5

Crawford, Fronefield, Victoria M. Kaspi, and Richard N. Manchester. "Radio Polarimetry Results for Young Southern Pulsars." International Astronomical Union Colloquium 177 (2000): 247–48. http://dx.doi.org/10.1017/s0252921100059601.

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AbstractWe present radio polarimetry results for nine Southern pulsars. Six of the nine are young, with characteristic ages less than 100 kyr and high spin-down luminosities. All six show significant linear polarization, and we confirm a previously noticed trend in which the degree of linear polarization increases with spin-down luminosity. We have used the rotating vector model to fit the observed position angle data for PSR J1513–5908 (B1509–58). We find that a magnetic inclination angleα> 60° is excluded at the 3σlevel in the fit, and that the geometry suggested by the morphology of an apparent bipolar X-ray outflow is marginally inconsistent with a recent model of the pulsar magnetosphere.

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6

von Hoensbroech, A., and K. M. Xilouris. "Multi-Frequency Pulsar Polarimetry at High Frequencies." International Astronomical Union Colloquium 160 (1996): 267–68. http://dx.doi.org/10.1017/s0252921100041683.

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AbstractA sample of 62 pulsar profiles has been studied with full polarization information at high radio frequencies, aiming at studying the dependency of emission altitude at the deepest layers of pulsar magnetospheres. The emission is consistent with heights ranging between 1-2% of the light-cylinder-radius, while a slight radius-to-frequency mapping is evident.

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7

Poutanen, Juri. "Relativistic rotating vector model for X-ray millisecond pulsars." Astronomy & Astrophysics 641 (September 2020): A166. http://dx.doi.org/10.1051/0004-6361/202038689.

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The X-ray radiation produced on the surface of accreting magnetised neutron stars is expected to be strongly polarised. A swing of the polarisation vector with the pulsar phase gives a direct measure of the source inclination and magnetic obliquity. In the case of rapidly rotating millisecond pulsars, the relativistic motion of the emission region causes additional rotation of the polarisation plane. Here, we develop a relativistic rotating vector model, where we derive analytical expression for the polarisation angle as a function of the pulsar phase accounting for relativistic aberration and gravitational light bending in the Schwarzschild metric. We show that in the case of fast pulsars the rotation of the polarisation plane can reach tens of degrees, strongly influencing the observed shape of the polarisation angle’s phase dependence. The rotation angle grows nearly linearly with the spin rate but it is less sensitive to the neutron star radius. Overall, this angle is large even for large spots. Our results have implications with regard to the modelling of X-ray polarisation from accreting millisecond pulsars that are to be observed with the upcoming Imaging X-ray Polarimeter Explorer and the enhanced X-ray Timing and Polarimetry mission. The X-ray polarisation may improve constraints on the neutron star mass and radius coming from the pulse profile modelling.

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8

O’Connor, Eoin G. P., Andrew Shearer, Christian Gouiffes, and Philippe Laurent. "High Time Resolution Astronomical Polarimetry with GASP." Proceedings of the International Astronomical Union 13, S337 (September 2017): 384–85. http://dx.doi.org/10.1017/s1743921317010626.

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AbstractThe Galway Astronomical Stokes Polarimeter (GASP) is a high time resolution, full-Stokes imaging polarimeter which utilises a Fresnel rhomb prism as a beam-splitter and quarter wave retarder. The ability to perform optical photometry and polarimetry at high frame rates enables more detailed studies of a multitude of compact objects including; optical pulsars, magnetars and Active Galactic Nuclei (AGN). We present a brief discussion of the instruments’ current capabilities and hardware design. GASP is currently configured with two Electron Multiplying Charge-Coupled Devices (EMCCDs), which offer sub-millisecond frame readout speeds over a defined region of interest on the sensor. We will report results from an observational campaign at the William Herschel Telescope (WHT) in December, 2015. During this campaign GASP was used to study the Crab Pulsar, V404 Cygni and polarisation standards. As a subset of our analysis we have identified a significant contribution from the Interstellar Medium (ISM) and the interaction of a varying polarised source with the ISM, the subsequent conversion of linearly polarised light to circular, and its dependence on the angle of the source emission electric field orientation. Further to the presentation of results we will discuss future observational work, which is planned for September 2017 and subsequent improvements to increase the temporal resolution of the detectors.

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9

Moran, Paul, Andy Shearer, and Roberto Mignani. "Optical Polarimetry of the Crab Nebula." Proceedings of the International Astronomical Union 7, S285 (September 2011): 379–81. http://dx.doi.org/10.1017/s1743921312001135.

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AbstractTime-resolved polarisation measurements of pulsars provide an unique insight into the geometry of the emission regions. Hubble Space Telescope (HST) polarisation data of the Crab Nebula were obtained from the Multimission Archive at STScI (MAST). The data are composed of a series of observations of the Crab Nebula with the HST and ACS camera system taken in three different polarisation filters (0°, 60° and 120°) between 2003 August and 2005 December. Polarisation vector maps of the Nebula were produced with the polarimetry software IMPOL. The degree of polarisation (P.D.) and the position angle (P.A.) of the pulsar's integrated pulse beam were measured, and also that of the nearby Synchrotron Knot, yielding P.D. = 4.90 ± 0.33 %, P.A. = 106°.46 ± 1°.9 for the pulsar, and P.D. = 61.70 ± 0.72 %, P.A. = 126°.86 ± 0°.23 for the Synchrotron Knot. These results are consistent with those of obtained by others using INTEGRAL.

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10

Kern, Jeffrey S., Timothy H. Hankins, and Joanna M. Rankin. "Single Pulse Polarimetry of the Vela Pulsar." International Astronomical Union Colloquium 177 (2000): 257–60. http://dx.doi.org/10.1017/s0252921100059649.

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AbstractMulti-frequency, single-pulse polarimetric observations of the Vela pulsar have been made using the VLA. These high time resolution measurements allow us to probe the geometry, and the time dependent characteristics of the radio emission region. Evidence for multiple emission components with differing spectral indices is found.

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11

Caiazzo, Ilaria, and Jeremy Heyl. "Polarization of accreting X-ray pulsars. I. A new model." Monthly Notices of the Royal Astronomical Society 501, no. 1 (November 5, 2020): 109–28. http://dx.doi.org/10.1093/mnras/staa3428.

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ABSTRACT A new window is opening in high-energy astronomy: X-ray polarimetry. With many missions currently under development and scheduled to launch as early as 2021, observations of the X-ray polarization of accreting X-ray pulsars will soon be available. As polarization is particularly sensitive to the geometry of the emission region, the upcoming polarimeters will shed new light on the emission mechanism of these objects, provided that we have sound theoretical models that agree with current spectroscopic and timing observation and that can make predictions of the polarization parameters of the emission. We here present a new model for the polarized emission of accreting X-ray pulsars in the accretion column scenario that for the first time takes into account the macroscopic structure and dynamics of the accretion region and the propagation of the radiation towards the observer, including relativistic beaming, gravitational lensing, and quantum electrodynamics. In this paper, we present all the details of the model, while in a companion paper, we apply our model to predict the polarization parameters of the bright X-ray pulsar Hercules X-1.

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12

Oswald, Lucy, Aris Karastergiou, and Simon Johnston. "Pulsar polarimetry with the Parkes ultra-wideband receiver." Monthly Notices of the Royal Astronomical Society 496, no. 2 (June 9, 2020): 1418–29. http://dx.doi.org/10.1093/mnras/staa1597.

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ABSTRACT Pulsar radio emission and its polarization are observed to evolve with frequency. This frequency dependence is key to the emission mechanism and the structure of the radio beam. With the new ultra-wideband receiver (UWL) on the Parkes radio telescope we are able, for the first time, to observe how pulsar profiles evolve over a broad continuous bandwidth of 700–4000 MHz. We describe here a technique for processing broad-band polarimetric observations to establish a meaningful alignment and visualize the data across the band. We apply this to observations of PSRs J1056–6258 and J1359–6038, chosen due to previously unresolved questions about the frequency evolution of their emission. Application of our technique reveals that it is possible to align the polarization position angle (PA) across a broad frequency range when constrained to applying only corrections for dispersion and Faraday rotation to do so. However, this does not correspond to aligned intensity profiles for these two sources. We find that it is possible to convert these misalignments into emission height range estimates that are consistent with published and simulated values, suggesting that they can be attributed to relativistic effects in the magnetosphere. We discuss this work in the context of the radio beam structure and prepare the ground for a wider study of pulsar emission using broad-band polarimetric data.

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13

You, X. P., R. N. Manchester, W. A. Coles, G. B. Hobbs, and R. Shannon. "Polarimetry of the Eclipsing Pulsar PSR J1748–2446A." Astrophysical Journal 867, no. 1 (October 25, 2018): 22. http://dx.doi.org/10.3847/1538-4357/aadee0.

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14

van Straten, W. "Radio Astronomical Polarimetry and High‐Precision Pulsar Timing." Astrophysical Journal 642, no. 2 (May 10, 2006): 1004–11. http://dx.doi.org/10.1086/501001.

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15

Xilouris, Kiriaki M., Michael Kramer, Axel Jessner, Alexis von Hoensbroech, Duncan R. Lorimer, Richard Wielebinski, Alexander Wolszczan, and Fernando Camilo. "The Characteristics of Millisecond Pulsar Emission. II. Polarimetry." Astrophysical Journal 501, no. 1 (July 1998): 286–306. http://dx.doi.org/10.1086/305791.

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16

Keith, M. J., S. Johnston, M. Bailes, S. D. Bates, N. D. R. Bhat, M. Burgay, S. Burke-Spolaor, et al. "The High Time Resolution Universe Pulsar Survey - IV. Discovery and polarimetry of millisecond pulsars." Monthly Notices of the Royal Astronomical Society 419, no. 2 (November 3, 2011): 1752–65. http://dx.doi.org/10.1111/j.1365-2966.2011.19842.x.

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17

Moran, P., A. Shearer, R. P. Mignani, A. Słowikowska, A. De Luca, C. Gouiffès, and P. Laurent. "Optical polarimetry of the inner Crab nebula and pulsar." Monthly Notices of the Royal Astronomical Society 433, no. 3 (June 20, 2013): 2564–75. http://dx.doi.org/10.1093/mnras/stt931.

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18

Moran, P., R. P. Mignani, and A. Shearer. "HST optical polarimetry of the Vela pulsar and nebula." Monthly Notices of the Royal Astronomical Society 445, no. 1 (September 30, 2014): 835–44. http://dx.doi.org/10.1093/mnras/stu1791.

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19

Brinkman, Casey, Paulo C. C. Freire, Joanna Rankin, and Kevin Stovall. "No pulsar left behind – I. Timing, pulse-sequence polarimetry and emission morphology for 12 pulsars." Monthly Notices of the Royal Astronomical Society 474, no. 2 (November 2, 2017): 2012–27. http://dx.doi.org/10.1093/mnras/stx2842.

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20

Morello, V., E. F. Keane, T. Enoto, S. Guillot, W. C. G. Ho, A. Jameson, M. Kramer, et al. "The SUrvey for Pulsars and Extragalactic Radio Bursts – IV. Discovery and polarimetry of a 12.1-s radio pulsar." Monthly Notices of the Royal Astronomical Society 493, no. 1 (February 5, 2020): 1165–77. http://dx.doi.org/10.1093/mnras/staa321.

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ABSTRACT We report the discovery of PSR J2251−3711, a radio pulsar with a spin period of 12.1 s, the second longest currently known. Its timing parameters imply a characteristic age of 15 Myr, a surface magnetic field of 1.3 × 1013 G, and a spin-down luminosity of 2.9 × 1029 erg s−1. Its dispersion measure of 12.12(1) pc cm−3 leads to distance estimates of 0.5 and 1.3 kpc according to the NE2001 and YMW16 Galactic free electron density models, respectively. Some of its single pulses show an uninterrupted 180-deg sweep of the phase-resolved polarization position angle, with an S-shape reminiscent of the rotating vector model prediction. However, the fact that this sweep occurs at different phases from one pulse to another is remarkable and without straightforward explanation. Although PSR J2251−3711 lies in the region of the $P-\dot{P}$ parameter space occupied by the X-ray isolated neutron stars (XINS), there is no evidence for an X-ray counterpart in our Swift XRT observation; this places a 99 per cent-confidence upper bound on its unabsorbed bolometric thermal luminosity of $1.1 \times 10^{31}~(d / 1~\mathrm{kpc})^2~\mathrm{erg\, s}^{-1}$ for an assumed temperature of 85 eV, where d is the distance to the pulsar. Further observations are needed to determine whether it is a rotation-powered pulsar with a true age of at least several Myr, or a much younger object such as an XINS or a recently cooled magnetar. Extreme specimens like PSR J2251−3711 help bridge populations in the so-called neutron star zoo in an attempt to understand their origins and evolution.

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21

Weisberg, J. M., J. M. Cordes, B. Kuan, K. E. Devine, J. T. Green, and D. C. Backer. "Arecibo 430 MHz Pulsar Polarimetry: Faraday Rotation Measures and Morphological Classifications." Astrophysical Journal Supplement Series 150, no. 1 (January 2004): 317–41. http://dx.doi.org/10.1086/379802.

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22

Michel, F. C., P. A. Scowen, R. J. Dufour, and J. J. Hester. "Observation of a pulsar wind - CCD polarimetry of the Crab Nebula." Astrophysical Journal 368 (February 1991): 463. http://dx.doi.org/10.1086/169710.

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23

Mignani, R. P., P. Moran, A. Shearer, V. Testa, A. Słowikowska, B. Rudak, K. Krzeszowki, and G. Kanbach. "VLT polarimetry observations of the middle-aged pulsar PSR B0656+14." Astronomy & Astrophysics 583 (November 2015): A105. http://dx.doi.org/10.1051/0004-6361/201527082.

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24

Bucciantini, Niccolò. "Future X-ray Polarimetry of Relativistic Accelerators: Pulsar Wind Nebulae and Supernova Remnants." Galaxies 6, no. 2 (March 27, 2018): 42. http://dx.doi.org/10.3390/galaxies6020042.

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25

van Straten, W. "HIGH-FIDELITY RADIO ASTRONOMICAL POLARIMETRY USING A MILLISECOND PULSAR AS A POLARIZED REFERENCE SOURCE." Astrophysical Journal Supplement Series 204, no. 1 (January 1, 2013): 13. http://dx.doi.org/10.1088/0067-0049/204/1/13.

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26

Vadawale, S. V., T. Chattopadhyay, N. P. S. Mithun, A. R. Rao, D. Bhattacharya, A. Vibhute, V. B. Bhalerao, et al. "Phase-resolved X-ray polarimetry of the Crab pulsar with the AstroSat CZT Imager." Nature Astronomy 2, no. 1 (November 6, 2017): 50–55. http://dx.doi.org/10.1038/s41550-017-0293-z.

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27

Suleymanova, Svetlana A., and V. D. Pugachev. "A Decade of Low Frequency Pulsar Polarimetry at PRAO: a Review of the Main Results." International Astronomical Union Colloquium 177 (2000): 201–4. http://dx.doi.org/10.1017/s0252921100059479.

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AbstractThe main results of the linear polarization measurements of pulsars done at the lowest radio frequencies 40, 60 and 103 MHz are summarized in this paper. We have analyzed 35 integrated polarization profiles and 20 statistical distribution displays and compared them with published high frequency results.

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28

Weisberg, J. M., J. E. Everett, J. M. Cordes, J. J. Morgan, and D. G. Brisbin. "A SEARCH FOR NEUTRON STAR PRECESSION AND INTERSTELLAR MAGNETIC FIELD VARIATIONS VIA MULTIEPOCH PULSAR POLARIMETRY." Astrophysical Journal 721, no. 2 (September 7, 2010): 1044–55. http://dx.doi.org/10.1088/0004-637x/721/2/1044.

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29

McKinnon, Mark M. "Statistical Modeling of the Circular Polarization in Pulsar Radio Emission and Detection Statistics of Radio Polarimetry." Astrophysical Journal 568, no. 1 (March 20, 2002): 302–11. http://dx.doi.org/10.1086/338843.

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30

Vadawale, S. V., T. Chattopadhyay, N. P. S. Mithun, A. R. Rao, D. Bhattacharya, A. Vibhute, V. B. Bhalerao, et al. "Author Correction: Phase-resolved X-ray polarimetry of the Crab pulsar with the AstroSat CZT Imager." Nature Astronomy 2, no. 5 (March 27, 2018): 428. http://dx.doi.org/10.1038/s41550-018-0425-0.

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31

Navarro, José, and R. N. Manchester. "Polarimetric Observations of PSR J0437–4715." International Astronomical Union Colloquium 160 (1996): 249–51. http://dx.doi.org/10.1017/s0252921100041622.

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To date there have been few polarimetric observations of millisecond pulsars, mainly due to the instrumental challenge of simultaneous high time resolution and large bandwidth. Such observations provide our most direct clues to the structure of the magnetic fields around pulsars, and are especially important in the case of millisecond pulsars, where radio emission necessarily originates very close to the neutron star surface.We have observed the bright millisecond pulsar J0437–4715 at the Parkes Radiotelescope with the Caltech Fast Pulsar Timing Machine, at several radio frequencies and in full polarimetric mode. Our analyses show significant deviations from the standard dipole field geometry.

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32

Osłowski, S., W. van Straten, M. Bailes, A. Jameson, and G. Hobbs. "Timing, polarimetry and physics of the bright, nearby millisecond pulsar PSR J0437−4715 – a single-pulse perspective." Monthly Notices of the Royal Astronomical Society 441, no. 4 (May 27, 2014): 3148–60. http://dx.doi.org/10.1093/mnras/stu804.

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33

Baglio, M. C., P. D’Avanzo, S. Campana, F. Coti Zelati, S. Covino, and D. M. Russell. "Different twins in the millisecond pulsar recycling scenario: Optical polarimetry of PSR J1023+0038 and XSS J12270-4859." Astronomy & Astrophysics 591 (June 22, 2016): A101. http://dx.doi.org/10.1051/0004-6361/201628383.

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34

Desvignes, Gregory, Michael Kramer, Kejia Lee, Joeri van Leeuwen, Ingrid Stairs, Axel Jessner, Ismaël Cognard, Laura Kasian, Andrew Lyne, and Ben W. Stappers. "Radio emission from a pulsar’s magnetic pole revealed by general relativity." Science 365, no. 6457 (September 5, 2019): 1013–17. http://dx.doi.org/10.1126/science.aav7272.

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Binary pulsars are affected by general relativity (GR), causing the spin axis of each pulsar to precess. We present polarimetric radio observations of the pulsar PSR J1906+0746 that demonstrate the validity of the geometrical model of pulsar polarization. We reconstruct the (sky-projected) polarization emission map over the pulsar’s magnetic pole and predict the disappearance of the detectable emission by 2028. Two tests of GR are performed using this system, including the spin precession for strongly self-gravitating bodies. We constrain the relativistic treatment of the pulsar polarization model and measure the pulsar beaming fraction, with implications for the population of neutron stars and the expected rate of neutron star mergers.

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35

Xilouris, Kiriaki M., Joanna M. Rankin, John H. Seiradakis, and Wolfgang Sieber. "Polarimetric Observations of 20 Weak Pulsars at 1720 Mhz." International Astronomical Union Colloquium 128 (1992): 165–71. http://dx.doi.org/10.1017/s0002731600155015.

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We present average polarization profiles for 20 pulsars at 1720 MHz made with the 100-m Effelsberg radio telescope. All four Stokes parameters were appropriately delayed in a linear dedisperser to correct the interstellar dispersion on-line. Our sample includes a number of complex profiles which were observed polarimetrically for the first time at a high frequency, with the aim of describing their frequency evolution. Classification of the corrected profiles is attempted according to the empirical pulsar model described earlier by Rankin(1990).

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36

Abbate, F., A. Possenti, C. Tiburzi, W. van Straten, E. Barr, A. Ridolfi, and P. Freire. "Polarization study of the pulsars in the globular cluster 47 Tucanae." Proceedings of the International Astronomical Union 13, S337 (September 2017): 295–98. http://dx.doi.org/10.1017/s1743921317008389.

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AbstractThe linearly polarized component of a pulsar signal at different radio frequencies can help to constrain the parallel component of the magnetic field along the line of sight. In this work we measured the polarimetric properties of the pulsars in the globular cluster 47 Tucanae and we report the Rotation Measure (RM) for 13 of them. A gradient in the RM values of the pulsars across the cluster is detected suggesting the presence of significant variations in the magnetic field across the very small angular scales associated with the lines of sight to the pulsars in 47 Tucanae. Both magnetic fields located in the globular cluster or in the Galactic disk in the direction of the cluster are taken into consideration. However, more detailed modelling of the dynamics of the cluster and deeper observations with the MeerKAT and/or the SKA1 radio telescopes are necessary to discriminate among the models.

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37

Thorsett, Stephen E., and Daniel R. Stinebring. "Polarimetry of millisecond pulsars." Astrophysical Journal 361 (October 1990): 644. http://dx.doi.org/10.1086/169226.

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38

Rahaman, S. k. Minhajur, Rahul Basu, Dipanjan Mitra, and George I. Melikidze. "Mode changing, subpulse drifting, and nulling in four component conal pulsar PSR J2321+6024." Monthly Notices of the Royal Astronomical Society 500, no. 3 (November 12, 2020): 4139–52. http://dx.doi.org/10.1093/mnras/staa3518.

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ABSTRACT In this study, we report on a detailed single pulse polarimetric analysis of the radio emission from the pulsar J2321+6024 (B2319+60) observed with the Giant Metrewave Radio Telescope, over wide frequencies ranging between 300 to 500 MHz and widely separated observing sessions. The pulsar profile shows the presence of four distinct conal components and belongs to a small group of pulsars classified as a conal quadrupole profile type. The single pulse sequence reveals the presence of three distinct emission modes, A, B, and ABN showing subpulse drifting. Besides, there were sequences when the pulsar did not show any drifting behaviour suggesting the possibility of a new emission state, which we have termed as mode C. The evolution of the mode changing behaviour was seen during the different observing sessions with different abundance as well as the average duration of the modes seen on each date. The drifting periodicities were 7.8 ± 0.3 P, 4.3 ± 0.4 P, and 3.1 ± 0.2 P in the modes A, B, and ABN, respectively, and showed large phase variations within the mode profile. The pulsar also showed the presence of orthogonal polarization modes, particularly in the leading and trailing components, which has different characteristics for the stronger and weaker pulses. However, no correlation was found between the emission modes and their polarization behaviour, with the estimated emission heights remaining roughly constant throughout. We have used the Partially Screened Gap model to understand the connection between drifting, mode changing, and nulling.

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39

Britton, M. C., W. van Straten, M. Bailes, M. Toscano, and R. N. Manchester. "High Precision Timing of PSR J0437–4715." International Astronomical Union Colloquium 177 (2000): 73–76. http://dx.doi.org/10.1017/s0252921100059066.

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AbstractSystematic effects currently dominate the timing residuals of the pulsar PSR J0437–4715. These systematics arise from transformations that occur during the propagation and detection of radio waves. The transformation properties of polarized radiation are related to the Lorentz group, and such effects may be represented using Lorentz transformations. These effects may be removed using the techniques of polarimetric self-calibration. Alternatively, an invariant profile may be formed from the polarimetric analogue of the Lorentz invariantI2–Q2–U2–V2and used for pulsar timing. Observations of PSR J0437–4715 are presented that show the consistency between these two techniques.

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Schnitzeler, D. H. F. M., R. P. Eatough, K. Ferrière, M. Kramer, K. J. Lee, A. Noutsos, and R. M. Shannon. "Radio polarimetry of Galactic Centre pulsars." Monthly Notices of the Royal Astronomical Society 459, no. 3 (April 13, 2016): 3005–11. http://dx.doi.org/10.1093/mnras/stw841.

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Gould, D. M., and A. G. Lyne. "Multifrequency polarimetry of 300 radio pulsars." Monthly Notices of the Royal Astronomical Society 301, no. 1 (November 1998): 235–60. http://dx.doi.org/10.1046/j.1365-8711.1998.02018.x.

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Stairs, I. H., S. E. Thorsett, and F. Camilo. "Coherently Dedispersed Polarimetry of Millisecond Pulsars." Astrophysical Journal Supplement Series 123, no. 2 (August 1999): 627–38. http://dx.doi.org/10.1086/313245.

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Mitra, Dipanjan, Rahul Basu, George I. Melikidze, and Mihir Arjunwadkar. "A single spark model for PSR J2144−3933." Monthly Notices of the Royal Astronomical Society 492, no. 2 (December 28, 2019): 2468–80. http://dx.doi.org/10.1093/mnras/stz3620.

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ABSTRACT The partially screened vacuum gap model (PSG) for the inner acceleration region in normal radio pulsars, a variant of the pure vacuum gap model, attempts to account for the observed thermal X-ray emission from polar caps and the subpulse drifting time-scales. We have used this model to explain the presence of death lines and extreme location of PSR J2144−3933 in the $P{-}\dot{P}$ diagram. This model requires maintaining the polar cap near a critical temperature and the presence of non-dipolar surface magnetic field to form the inner acceleration region. In the PSG model, thermostatic regulation is achieved by sparking discharges, which are a feature of all vacuum gap models. We demonstrate that non-dipolar surface magnetic field reduces polar cap area in PSR J2144−3933 such that only one spark can be produced and is sufficient to sustain the critical temperature. This pulsar has a single-component profile over a wide frequency range. Single-pulse polarimetric observations and the rotating vector model confirm that the observer’s line of sight traverses the emission beam centrally. These observations are consistent with a single spark operating within framework of the PSG model leading to single-component emission. Additionally, single-pulse modulations of this pulsar, including lack of subpulse drifting, presence of single-period nulls and microstructure, are compatible with a single spark either in PSG or in general vacuum gap models.

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Shrauner, J. A., I. H. Stairs, R. J. Dewey, M. Krumholz, H. E. Taylor, J. H. Taylor, and S. E. Thorsett. "Mark IV: A Phase Coherent Observing System for Pulsars." International Astronomical Union Colloquium 160 (1996): 23–24. http://dx.doi.org/10.1017/s0252921100040938.

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We have built a new radio astronomical receiving system designed specifically for very high precision timing and polarimetry of fast pulsars. Unlike most detectors currently used to study pulsars, this intrument does not square the received signal at the time of observation. Instead, voltages proportional to the instantaneous electric vectors of incoming signals are digitized, time-tagged, and recorded on high speed magnetic media. We have tested the system using a 5 MHz bandwidth signal with 2-bit digitization at the Greenbank 140 foot telescope. Full polarization information was obtained with a 0.2μs time resolution. We have used this system to study the giant pulses emitted by PSR B0531+21 and PSR B1937+21, to determine high precision dispersion measures, and to perform high precision timing and polarimetry.

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Olszanski, Timothy E. E., Dipanjan Mitra, and Joanna M. Rankin. "Arecibo 4.5/1.4/0.33-GHz polarimetric single-pulse emission survey." Monthly Notices of the Royal Astronomical Society 489, no. 2 (August 12, 2019): 1543–55. http://dx.doi.org/10.1093/mnras/stz2172.

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ABSTRACT We report on an Arecibo 4.5-GHz polarimetric single-pulse survey of the brightest pulsars at high frequency within its sky. The high-frequency profiles are accompanied by a collection of both previously published and unpublished high quality 1.4- and 0.33-GHz observations. Here our analyses and discussion primarily involve the average and statistical properties of the 46 pulsars polarimetric pulse sequences, profile classification and frequency evolution, and polarimetric profiles and peak-occurrence histograms. In most cases both the fractional linear polarization and profile widths decrease with frequency as expected, but there are some exceptions. Similarly, we were able to review and/or extend the profile classifications for this population of pulsars and work out their beaming characteristics quantitatively showing that almost all show properties compatible with the core/double-cone emission beam model. The entirety of these observations’ average profiles are accessible for download.

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Kern, Jeffrey S. "Single Pulse Analysis of the Core-Dominated Pulsar B0611+22." International Astronomical Union Colloquium 177 (2000): 175–76. http://dx.doi.org/10.1017/s0252921100059388.

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AbstractSingle pulse studies of pulsar radio emission provide a window into the time dependent behavior of the radio loud region. I have analyzed a series of precision polarimetric observations of pulsar B0611+22 to determine the geometry of the emission region. The observations are consistent with a central core emission region, and a periodically present conal component. This identification leads to the surprising result that all emission is from the leading half of the polar cap.

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Rankin, Joanna M. "Pulsar Polarization, Emission, and Beaming." International Astronomical Union Colloquium 160 (1996): 237–44. http://dx.doi.org/10.1017/s0252921100041609.

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AbstractThis paper discusses observational and analytical questions pertaining to the pulsar emission problem. A short outline of the area is given for those new to the subject. Some of the literature pertinent to pulsar polarization, emission and beaming, which has appeared over about the last five years is mentioned. There is a short discussion of efforts to carry out polarimetric observations of higher quality, and finally, there is a short discussion of recent work by the author and her colleagues.

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GOULD, D. M. "Polarization in Pulsar Radio Emission." International Astronomical Union Colloquium 128 (1992): 384–86. http://dx.doi.org/10.1017/s0002731600155581.

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Polarimetric observations of over 300 pulsars have been carried out between 21 December 1988 and 22 January 1990 at 606, 610, 925, and 1408 MHz using the Lovell Telescope at Jodrell Bank. Many of these pulsars have no previously published polarization profiles and will be published shortly (Gould and Lyne 1990). This large data set along with previously published data from various sources, has been used to test the correlation found by Radhakrishnan and Rankin (1990) between sense reversing circular polarization signatures and the accompanying sense of rotation of the linear polarization position angle.

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Karastergiou, A., A. Jessner, and R. Wielebinski. "High-frequency Polarimetric Observations of the Crab Pulsar." Symposium - International Astronomical Union 218 (2004): 329–30. http://dx.doi.org/10.1017/s0074180900181288.

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We present high quality polarimetric observations with the Effelsberg radio telescope of the Crab pulsar at 8.35 GHz using a new sensitive receiver with a very large bandwidth. We present our observations and discuss them in the context of the conclusions reached by Moffett & Hankins (1999) about the geometry and the origin of the various pulse components.

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Ord, S. M., W. van Straten, A. W. Hotan, and M. Bailes. "Polarimetric profiles of 27 millisecond pulsars." Monthly Notices of the Royal Astronomical Society 352, no. 3 (August 11, 2004): 804–14. http://dx.doi.org/10.1111/j.1365-2966.2004.07963.x.

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