Radio Observations of Two Intermittent Pulsars: PSRs J1832+0029 and J1841−0500

Wang, S. Q.; Wang, J. B.; Hobbs, G.; Zhang, S.B.; Shannon, R. M.; Dai, Shi; Hollow, Robert; Kerr, M.; Ravi, Vikram; Wang, N.; Zhang, L.

doi:10.3847/1538-4357/ab9302

Cited by 12 publications

(4 citation statements)

References 31 publications

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“…This is similar to the mode switching time-scales found in normal, non-millisecond pulsars (but note these time scales are much shorter than the pulse variations identified for intermittent pulsars; e.g. Wang et al 2020).…”

Section: Moding-changingsupporting

confidence: 80%

A single pulse study of PSR J1022+1001

Feng,

Hobbs,

et al. 2020

Preprint

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Using the Five-hundred-meter Aperture Spherical radio Telescope (FAST), we have recorded ∼ 10 5 single pulses from PSR J1022+1001. We studied the polarization properties, their energy distribution and their times of arrival. This is only possible with the high sensitivity available using FAST. There is no indication that PSR J1022+1001 exhibits giant pulse, nulling or traditional mode changing phenomena. The energy in the leading and trailing components of the integrated profile is shown to be correlated. The degree of both linear and circular polarization increases with the pulse flux density for individual pulses. Our data indicates that pulse jitter leads to an excess noise in the timing residuals of 67 ns when scaled to one hour, which is consistent with Liu et al. (2015). We have unsuccessfully trialled various methods to improve timing precision through the selection of specific single pulses. Our work demonstrates that FAST can detect individual pulses from pulsars that are observed in order to detect and study gravitational waves. This capability enables detailed studies, and parameterisation, of the noise processes that affect the sensitivity of a pulsar timing array.

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Section: Moding-changingsupporting

confidence: 80%

A single pulse study of PSR J1022+1001

Feng,

Hobbs,

et al. 2020

Preprint

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“…It is interesting that in all previous solutions of the FFE pulsar magnetosphere, the above ratio was found to be greater than 3 (e.g., [22]). This value is significantly larger than the ratio of spindown rates ĖON / ĖOFF observed in the intermittent pulsars PSR B1931+24, PSR J1832+0029 and PSR J1841-0500 for their corresponding 'ON' and 'OFF' states (1.5, 1.7 and 2.5, respectively, e.g., [23,24]). The inability to account for observed values lower than 3 was the reason that led to the development of resistive magnetospheric solutions (e.g., [22,25]).…”

Section: A Spectrum Of Solutionsmentioning

confidence: 64%

A New Solution of the Pulsar Equation

Contopoulos,

Dimitropoulos,

Ntotsikas

et al. 2024

Universe

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We present the first new type of solution of the pulsar equation since 1999. In it, the whole magnetosphere is confined inside the light cylinder and an electrically charged layer wraps around it and holds it together. The reason this new solution has never been obtained before is that all current time-dependent simulations are initialized with a vacuum dipole configuration that extends to infinity; thus, their final steady-state solution also extends to infinity. Under special conditions, such a confined configuration may be attained when the neutron star first forms in the interior of a collapsing star during a supernova explosion, or when it accretes from an external wind or disk from a donor star. It is shown that this new maximally closed non-decelerating solution is the limit of a continuous sequence of standard magnetospheres with open and closed field lines when the amount of open field lines gradually drops to zero. The minimum energy solution in this sequence is a standard magnetosphere in which the closed field line region extends up to about 80% of the light cylinder. We estimate that the released energy when the new solution transitions to the minimum energy one is enough to power a fast radio burst.

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“…Pulsar nulling and mode changing have been detected in many pulsars. The pulse nulling is a phenomenon that the pulse emission disappears abruptly for a few pulse periods to several hours, even to several years, and then turns on again (Ritchings 1976;Rankin 1986;Vivekanand 1995;Kramer et al 2006;Wang et al 2007;Camilo et al 2012;Wang et al 2020b). Mode changing is another emission phenomenon in which the average pulse profile switches between two or more states (Bartel & Hankins 1982).…”

Section: Introductionmentioning

confidence: 99%

Polarimetric Observations of PSR J0614+2229 and PSR J1938+2213 Using FAST

Sun

Yan

Wang

et al. 2022

ApJ

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We presented observations of PSRs J0614+2229 and J1938+2213 using the Five-hundred-meter Aperture Spherical radio Telescope. PSR J0614+2229 shows two distinct emission states, in which the emission of state A occurs earlier than that of state B in longitude. The phase offset between the average pulse profile peaks of the two states is about 1.°05. The polarization properties of the average pulse profile of the two states are different with different linear position angle swings. We found that the emission becomes brighter during the transition between the two states, which has never been seen in other mode-changing pulsars before. PSR J1938+2213 appears to consist of a weak emission state superposed by brighter burst emissions. The weak state is always present and the energy of the strongest pulse in the burst state is about 57 times larger than that of the average pulse energy. The polarization properties of the two states are also different, and orthogonal polarization modes can be seen only in the burst state, rather than both states. Our results suggest that, for the two pulsars, the emissions of the two states may be generated in different regions in the pulsar magnetosphere.

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Radio Observations of Two Intermittent Pulsars: PSRs J1832+0029 and J1841−0500

Cited by 12 publications

References 31 publications

A single pulse study of PSR J1022+1001

A single pulse study of PSR J1022+1001

A New Solution of the Pulsar Equation

Polarimetric Observations of PSR J0614+2229 and PSR J1938+2213 Using FAST

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