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Atmospheric Circulation on Black Widow Companions
High Energy Astrophysical Phenomena · Submitted 27 Feb 2020
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim These are among the highest masses known, and our improved modeling increases confidence that the results are important for understanding the dense matter equation of state.
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The abstract, sentence by sentence
We present a model for atmospheric wind circulation in binary millisecond pulsar (MSP) companions, showing how the optical light curve (LC) and radial velocities (RV) are sensitive to the wind flow, causing LC orbital phase shifts and asymmetries, as observed for several `spider' MSP. Velocity widths of spectral lines offer additional opportunities for measuring surface wind speed. As examples, we fit optical data for a black widow pulsar J1959+2048 and a redback pulsar J2215+5135; the wind heating models (WH) are statistically strongly preferred over direct heating (DH) for both objects, although the latter is even better fit with a heated spot. In general, WH effects tend to increase the inferred orbital inclination $i$ and decrease the inferred companion center-of-mass radial velocity amplitude $K_\mathrm{c}$; both effects decrease the inferred neutron star mass. Even with such a decrease, we find large masses for the two neutron stars: $2.18\pm0.09M_\odot$ and $2.28^{+0.10}_{-0.09}M_\odot$, respectively (for the modest surface speeds fit from the bulk heat flow; supersonic photospheric winds can slightly change these values). These are among the highest masses known, and our improved modeling increases confidence that the results are important for understanding the dense matter equation of state.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present a model for atmospheric wind circulation in binary millisecond pulsar (MSP) companions, showing how the optical light curve (LC) and radial velocities (RV) are sensitive to the wind flow, causing LC orbital phase shifts and asymmetries, as observed for several `spider' MSP. | contribution 0.99 | 0.91 | 0.34 | asserted 1.00 |
| s1 | Velocity widths of spectral lines offer additional opportunities for measuring surface wind speed. | method 0.59 | 0.21 | 0.03 | hedged possibility 0.64 |
| s2 | As examples, we fit optical data for a black widow pulsar J1959+2048 and a redback pulsar J2215+5135; the wind heating models (WH) are statistically strongly preferred over direct heating (DH) for both objects, although the latter is even better fit with a heated spot. | result 0.74 | 0.95 | 0.14 | asserted 1.00 |
| s3 | In general, WH effects tend to increase the inferred orbital inclination $i$ and decrease the inferred companion center-of-mass radial velocity amplitude $K_\mathrm{c}$; both effects decrease the inferred neutron star mass. | result 0.53 | 0.67 | 0.13 | asserted 0.81 |
| s4 | Even with such a decrease, we find large masses for the two neutron stars: $2.18\pm0.09M_\odot$ and $2.28^{+0.10}_{-0.09}M_\odot$, respectively (for the modest surface speeds fit from the bulk heat flow; supersonic photospheric winds can slightly change these values). | result 1.00 | 0.96 | 0.27 | asserted 1.00 |
| s5 | These are among the highest masses known, and our improved modeling increases confidence that the results are important for understanding the dense matter equation of state. | interpretation 1.00 | 0.85 | 0.43 | asserted 0.91 |
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The paper
Original abstract
We present a model for atmospheric wind circulation in binary millisecond pulsar (MSP) companions, showing how the optical light curve (LC) and radial velocities (RV) are sensitive to the wind flow, causing LC orbital phase shifts and asymmetries, as observed for several `spider' MSP. Velocity widths of spectral lines offer additional opportunities for measuring surface wind speed. As examples, we fit optical data for a black widow pulsar J1959+2048 and a redback pulsar J2215+5135; the wind heating models (WH) are statistically strongly preferred over direct heating (DH) for both objects, although the latter is even better fit with a heated spot. In general, WH effects tend to increase the inferred orbital inclination $i$ and decrease the inferred companion center-of-mass radial velocity amplitude $K_\mathrm{c}$; both effects decrease the inferred neutron star mass. Even with such a decrease, we find large masses for the two neutron stars: $2.18\pm0.09M_\odot$ and $2.28^{+0.10}_{-0.09}M_\odot$, respectively (for the modest surface speeds fit from the bulk heat flow; supersonic photospheric winds can slightly change these values). These are among the highest masses known, and our improved modeling increases confidence that the results are important for understanding the dense matter equation of state.
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References
How the literature uses it
3 arXiv papers cite this in 14 sentences
Papers citing it · 4 sentences without a confident label
Contests it 1 paper
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Although this approach permits reasonable fits of some light curves [ref] , this model is unable to account for asymmetries between the leading and trailing edge of the companion (assuming a symmetric irradiation pattern) such as seen in, for example, the black widows PSR J2051-0827 [ref] and PSR B1957+20 [ref] or the redback PSR J2215+5135 [ref] .
A model for redistributing heat over the surface of irradiated spider companions · Introduction · contest 0.81
Uses its data or values 2 papers
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This data was initially presented in [ref] , and is also employed in [ref] .
A model for redistributing heat over the surface of irradiated spider companions · Application to PSR J2215+5135 · 0.98
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Based on atmospheric wind circulation modeling in binary MSP companions, Ref. [ref] reported the mass of PSR J1959+2048 to be $2.18±0.09 M_⊙$.
Dense Matter and Compact Stars in Strong Magnetic Fields · Dense matter inside neutron stars · 0.99
Compares with it 1 paper
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In particular, in [ref] it is found that $w ≃35^∘$ ($θ_c$ in their notations) while we find $w > 90^∘$, rendering the model virtually equivalent to uniform convection.
A model for redistributing heat over the surface of irradiated spider companions · Convection · 0.89
Cites it as background 1 paper
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While cool star spots caused by magnetic activity are a plausible explanation for variability and asymmetry in the optical light curves [ref] , other mechanisms such as asymmetric heating from the pulsar [ref] , or heat re-distribution due to convective flows on the stellar surface [ref] , may also explain this.
Einstein@Home Discovery of the Gamma-ray Millisecond Pulsar PSR J2039-5617 Confirms Its Predicted Redback Nature · Light curve modelling · 0.84
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