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Study of spider pulsar binary eclipses and discovery of an eclipse mechanism transition
High Energy Astrophysical Phenomena · Submitted 4 Mar 2020
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim For PSR J1816+4510 we present the first direct evidence of an eclipse mechanism that transitions from one that removes the pulsar flux from the line of sight to one that merely smears out pulsations, and claim that this is a consequence of scattering in a tail of material flowing behind the companion.
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The abstract, sentence by sentence
We present a comparative study of the low-frequency eclipses of spider (compact, irradiating binary) PSRs B1957+20 and J1816+4510. Combining these data with those of three other eclipsing systems we study the frequency dependence of the eclipse duration. PSRs B1957+20 and J1816+4510 have similar orbital properties, but the companions to the pulsars have masses that differ by an order of magnitude. A dedicated campaign to simultaneously observe the pulsed and imaged continuum flux densities throughout the eclipses reveals many similarities between the excess material within the two binaries, irrespective of the companion star properties. The observations show that the pulsar fluxes are removed from the line of sight throughout the main body of the eclipses. For PSR J1816+4510 we present the first direct evidence of an eclipse mechanism that transitions from one that removes the pulsar flux from the line of sight to one that merely smears out pulsations, and claim that this is a consequence of scattering in a tail of material flowing behind the companion. Inferred mass loss rates from the companion stars are found to be $\dot{M}_{\text{C}} \sim 10^{-12}~M_\odot$~yr$^{-1}$ and $\dot{M}_{\text{C}} \sim 2 \times 10^{-13}~M_\odot$~yr$^{-1}$ for PSR B1957+20 and PSR J1816+4510, respectively; seemingly too low to evaporate the stars within Hubble time. Measurements of eclipse durations over a wide range of radio-frequencies show a significant dependence of eclipse duration on frequency for all pulsars, with wider eclipses at lower-frequencies. These results provide a marked improvement in the observational constraints available for theoretical studies of the eclipse mechanisms.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present a comparative study of the low-frequency eclipses of spider (compact, irradiating binary) PSRs B1957+20 and J1816+4510. | contribution 1.00 | 0.91 | 0.03 | asserted 0.85 |
| s1 | Combining these data with those of three other eclipsing systems we study the frequency dependence of the eclipse duration. | method 0.59 | 0.87 | 0.03 | asserted 0.56 |
| s2 | PSRs B1957+20 and J1816+4510 have similar orbital properties, but the companions to the pulsars have masses that differ by an order of magnitude. | background 0.85 | 0.42 | 0.04 | asserted 1.00 |
| s3 | A dedicated campaign to simultaneously observe the pulsed and imaged continuum flux densities throughout the eclipses reveals many similarities between the excess material within the two binaries, irrespective of the companion star properties. | result 0.81 | 0.94 | 0.12 | asserted 0.99 |
| s4 | The observations show that the pulsar fluxes are removed from the line of sight throughout the main body of the eclipses. | result 1.00 | 0.84 | 0.07 | asserted 1.00 |
| s5 | For PSR J1816+4510 we present the first direct evidence of an eclipse mechanism that transitions from one that removes the pulsar flux from the line of sight to one that merely smears out pulsations, and claim that this is a consequence of scattering in a tail of material flowing behind the companion. | result 0.56 | 0.96 | 0.69 | asserted 0.91 |
| s6 | Inferred mass loss rates from the companion stars are found to be $\dot{M}_{\text{C}} \sim 10^{-12}~M_\odot$~yr$^{-1}$ and $\dot{M}_{\text{C}} \sim 2 \times 10^{-13}~M_\odot$~yr$^{-1}$ for PSR B1957+20 and PSR J1816+4510, respectively; seemingly too low to evaporate the stars within Hubble time. | result 0.95 | 0.94 | 0.07 | asserted 0.79 |
| s7 | Measurements of eclipse durations over a wide range of radio-frequencies show a significant dependence of eclipse duration on frequency for all pulsars, with wider eclipses at lower-frequencies. | result 1.00 | 0.88 | 0.18 | asserted 1.00 |
| s8 | These results provide a marked improvement in the observational constraints available for theoretical studies of the eclipse mechanisms. | interpretation 0.88 | 0.53 | 0.13 | asserted 1.00 |
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The paper
Original abstract
We present a comparative study of the low-frequency eclipses of spider (compact, irradiating binary) PSRs B1957+20 and J1816+4510. Combining these data with those of three other eclipsing systems we study the frequency dependence of the eclipse duration. PSRs B1957+20 and J1816+4510 have similar orbital properties, but the companions to the pulsars have masses that differ by an order of magnitude. A dedicated campaign to simultaneously observe the pulsed and imaged continuum flux densities throughout the eclipses reveals many similarities between the excess material within the two binaries, irrespective of the companion star properties. The observations show that the pulsar fluxes are removed from the line of sight throughout the main body of the eclipses. For PSR J1816+4510 we present the first direct evidence of an eclipse mechanism that transitions from one that removes the pulsar flux from the line of sight to one that merely smears out pulsations, and claim that this is a consequence of scattering in a tail of material flowing behind the companion. Inferred mass loss rates from the companion stars are found to be $\dot{M}_{\text{C}} \sim 10^{-12}~M_\odot$~yr$^{-1}$ and $\dot{M}_{\text{C}} \sim 2 \times 10^{-13}~M_\odot$~yr$^{-1}$ for PSR B1957+20 and PSR J1816+4510, respectively; seemingly too low to evaporate the stars within Hubble time. Measurements of eclipse durations over a wide range of radio-frequencies show a significant dependence of eclipse duration on frequency for all pulsars, with wider eclipses at lower-frequencies. These results provide a marked improvement in the observational constraints available for theoretical studies of the eclipse mechanisms.
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References
How the literature uses it
2 arXiv papers cite this in 3 sentences
Papers citing it · 2 sentences without a confident label
Cites it as background 1 paper
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The continuum radio signal is diminished due to absorption, while scattering or dispersion makes the radio pulses challenging to detect (e.g., [ref] ).
The MAVERIC Survey: New compact binaries revealed by deep radio continuum observations of the Galactic globular cluster Terzan 5 · Introduction · 0.83
What it cites · 3 sentences without a confident label
Uses the method or tool of 2 papers
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These observations consisted of a 2 h LOFAR observation covering 110–188 MHz, a 2 h uGMRT observation covering 300–500 MHz and a 3 h Parkes Telescope observation covering 705–4032 MHz utilising the new ultra-wide-bandwidth low-frequency receiver [ref] .
An ultra-wide bandwidth (704 to 4032 MHz) receiver for the Parkes radio telescope · Observations · 0.96
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The complex-voltage LOFAR data for J1816 and B1957 were coherently dedispersed, folded and cleaned as part of the LOFAR Known Pulsar Pipeline [ref] .
The LOFAR Known Pulsar Data Pipeline · Beamformed data · 1.00
Cites as background 1 paper
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We note recent work by [ref] in which they model outflows from black widow companions considering thermal and dynamical processes in the wind.
Black widow evolution: magnetic braking by an ablated wind · Mass loss · 0.98
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