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

Shang, Lun-Hua; Lu, Jiguang; Du, Y. J.; Hao, Longfei; Li, Di; Lee, Kejia; Li, Bin; Li, Lixin; Qiao, G. J.; Shen, Zhi-Qiang; Wang, Dehua; Wang, Min; Wu, Xiaoguang; Wu, Yajun; Xu, R. X.; Yue, Youling; Yan, Zhen; Zhi, Qi‐Jun; Zhao, Rong-Bing; Zhao, Ru-Shuang

doi:10.1093/mnras/stx815

Cited by 16 publications

(5 citation statements)

References 69 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Here, P is three times of period of J0815+0939. Shang et al 2017Shang et al , 2021 for details), and find that the separations of the four components are 38.29 ± 0.66 ms, 69.88 ± 1.60 ms and 41.16 ± 1.15 ms at the 1250 MHz band, respectively. This is different from that in previous observation of 400 MHz.…”

Section: The Mean Pulse Profilesmentioning

confidence: 98%

The “Bi-drifting” Subpulses of PSR J0815+0939 Observed with the Five-hundred-meter Aperture Spherical Radio Telescope

Shang

Bai

Dang

et al. 2022

Res. Astron. Astrophys.

Self Cite

View full text Add to dashboard Cite

We report the “Bi-drifting” subpulses observed in PSR J0815+0939 using the Five-hundred-meter Aperture Spherical radio Telescope (FAST). The observation at band from 1050-1450MHz is evenly divided into two bands, i.e., the bands at center frequencies 1150MHz and 1350 MHz. The mean pulse profiles and the “Bi-drifting” subpulses at this two bands are investigated. It is found that the pulse profiles at this two frequencies show four emission components, and the peak separations between four emission components decrease with the increase of frequency. In addition, the ratio of peak intensity of each component to the intensity of component IV at 1150MHz is larger than that at 1350 MHz. We carry out an analysis of the longitude-resolved fluctuation spectrum and two-dimensional fluctuation spectrum for each emission component, and find that the P3 of components I, II and III are about 10.56, 10.57 and 10.59 s at 1150MHz and 1350 MHz. However, the reliable measurements of P3 of component IV and P2 for these four components were not obtained due to the low signal-to-noise ratio of observation data. The pulse energy distributions at frequencies 1150 and 1350MHz are presented, and it is found that no nulling phenomenon have been found in this pulsar. With our observation from the FAST, the “Bi-drifting” subpulse phenomenon of PSR J0815+0939 is expanded from 400MHz to 1350 MHz, which is helpful for the relevant researchers to test and constrain the pulsar emission model, especially the model of “Bi-drifting” subpulse.

show abstract

Section: The Mean Pulse Profilesmentioning

confidence: 98%

The “Bi-drifting” Subpulses of PSR J0815+0939 Observed with the Five-hundred-meter Aperture Spherical Radio Telescope

Shang

Bai

Dang

et al. 2022

Res. Astron. Astrophys.

Self Cite

View full text Add to dashboard Cite

show abstract

“…where ψ is the observed position angle, the impact angle & Manchester 1988;Zhang et al 2007;Shang et al 2017), and f is the longitude, defined to be zero on the magnetic meridian. Here ψ 0 and f 0 are offset from the position angle and phase, respectively.…”

Section: The Average Pulse Profilementioning

confidence: 99%

“…A pulsar is known for its highly periodic pulse emission. The shape of its mean pulse profile, which is folded by the single pulse, is usually very stable (Helfand et al 1975;Kramer et al 1994;Kramer 1994;Qiao et al 2001;Shang et al 2017Shang et al , 2020Shang et al , 2021. However, it is found that the single pulses, which represent the detailed emission process, are different from each other.…”

Section: Introductionmentioning

confidence: 99%

The Single-pulse Observation of PSR B2111+46 with the Five-hundred-meter Aperture Spherical Radio Telescope

Zhi,

Bai,

Shang

et al. 2023

ApJ

View full text Add to dashboard Cite

We report the observations of periodic nulling in PSR B2111+46 at 1250 MHz with the Five-hundred-meter Aperture Spherical radio Telescope (FAST). The nulling fractions (NF) as well as nulling period of this pulsar were calculated. The NF and nulling period are 17% ± 1% and 62.49 ± 0.99 P 1, respectively, and the periodic nulling shows variations in periodicity with time. The durations of each consecutive burst and nulling were investigated, which show that the power-law distribution and the indices are −1.11 ± 0.04 and −2.08 ± 0.23. In the observed frequency band, the width of the profile is narrowed with the increase in frequency, and the degree of polarization has no obvious trend with the increase in frequency. We discovered a weak emission component in front of the leading component of this triple-type profile pulsar that was not observed in other bands and by other telescopes. With the fitting of rotation vector model, we obtained that the angles of the magnetic inclination α and the line of sight ζ are ∼13.°0 and ∼11.°6, respectively. The high-sensitivity observation of FAST improves our understanding of the emission of this pulsar.

show abstract

“…Then the radiation beamwidth is ρ beam ≈ 7°.0 in this case, which is consistent with the observations. Later, we combine Equation (33) with r r r sin e 2 e 2 q q = » (for a small θ) and a frequency of curvature radiation It can be estimated from Figure 5 of Shang et al (2017) that r ≈ 155 km is where the radiation with a frequency of 2 GHz is generated. Using the data from PSR B0329+54 mentioned above, we find that the Lorentz factors are γ d ≈ 441 (this is consistent with the observation).…”

Section: Pure Dipole Fieldmentioning

confidence: 99%

Rotating Vector Model and Radius-to-frequency Mapping in the Presence of a Multipole Magnetic Field

Qiu,

Tong,

Wang

2023

ApJ

View full text Add to dashboard Cite

The rotating vector model and radius-to-frequency mapping in the presence of a multipole magnetic field in pulsars and magnetars are considered. An axisymmetric potential field is assumed, and the following is found: (1) The radiation beam in the case of a multipole field is wider than the dipole case. This may account for the increasing pulse width at the higher frequency of pulsars (anti-radius-to-frequency mapping); (2) The expression for the polarization position angle is unchanged. Only the inclination angle α and phase constant ϕ 0 will change. The angle between the rotational axis and line of sight and the position angle constant ψ 0 will not change. When fitting the varying position angle of magnetars, these constraints should be considered. The appearance and disappearance of a multipole field may account for the changing slope of the position angle in the radio-emitting magnetar Swift J1818.0–1607. A similar but more active process in magnetar magnetospheres may account for the diverse position angle in fast radio bursts.

show abstract

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

Cited by 16 publications

References 69 publications

The “Bi-drifting” Subpulses of PSR J0815+0939 Observed with the Five-hundred-meter Aperture Spherical Radio Telescope

The “Bi-drifting” Subpulses of PSR J0815+0939 Observed with the Five-hundred-meter Aperture Spherical Radio Telescope

The Single-pulse Observation of PSR B2111+46 with the Five-hundred-meter Aperture Spherical Radio Telescope

Rotating Vector Model and Radius-to-frequency Mapping in the Presence of a Multipole Magnetic Field

Contact Info

Product

Resources

About