Imprint of magnetic obliquity in apparent spin-down of radio pulsars

Anton Biryukov; Gregory Beskin

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Imprint of magnetic obliquity in apparent spin-down of radio pulsars

Anton Biryukov, Gregory Beskin

High Energy Astrophysical Phenomena · Submitted 16 May 2023

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim We found, that the apparent pulsar spin-down is consistent with the theory if assumed, that magnetic moments of orthogonal rotators are systematically larger than those of aligned ones for $\sim 0.15..0.2$ dex.

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What the abstract itself states, as probabilities: claims first 0.05 · states limitation 0.46 · human participants 0.02 · controlled comparison 0.74 · randomized assignment 0.02 · states quantitative result 0.98 · compares with prior results 0.49 · mentions code or data availability 0.02.

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arXiv listing abstract v1. Results and the main claim are underlined; show every role.

Numerical simulations predict that the spin-down rate of a single rotation-powered neutron star depends on the angle $\alpha$ between its spin and magnetic axes as $P\dot P \propto \mu^2 (k_0 + k_1\sin^2\alpha)$, where $P$ is the star spin period, $\mu$ is its magnetic moment, while $k_0 \sim k_1 \sim 1$. Here we describe a simple observational test for this prediction based on the comparison of spin-down rates of 50 nearly orthogonal (with $\alpha$ close to 90 deg) and 27 nearly aligned (with $\alpha$ close to 0 deg) pulsars. We found, that the apparent pulsar spin-down is consistent with the theory if assumed, that magnetic moments of orthogonal rotators are systematically larger than those of aligned ones for $\sim 0.15..0.2$ dex. Also, as a by-product of the analysis, we provide yet another constraint on the average braking index of radio pulsars as $1 \le n \le 4$ with formal significance not worse than 99\%.

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What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	Numerical simulations predict that the spin-down rate of a single rotation-powered neutron star depends on the angle $\alpha$ between its spin and magnetic axes as $P\dot P \propto \mu^2 (k_0 + k_1\sin^2\alpha)$, where $P$ is the star spin period, $\mu$ is its magnetic moment, while $k_0 \sim k_1 \sim 1$.	background 1.00	0.05	0.04	asserted 0.82
s1	Here we describe a simple observational test for this prediction based on the comparison of spin-down rates of 50 nearly orthogonal (with $\alpha$ close to 90 deg) and 27 nearly aligned (with $\alpha$ close to 0 deg) pulsars.	method 0.66	0.86	0.04	asserted 0.89
s2	We found, that the apparent pulsar spin-down is consistent with the theory if assumed, that magnetic moments of orthogonal rotators are systematically larger than those of aligned ones for $\sim 0.15..0.2$ dex.	result 0.97	0.97	0.86	hedged possibility 0.83
s3	Also, as a by-product of the analysis, we provide yet another constraint on the average braking index of radio pulsars as $1 \le n \le 4$ with formal significance not worse than 99\%.	result 1.00	0.92	0.06	asserted 1.00

What kind of paper the classifier reports this is: empirical study 0.99 · evidence from analysis of existing data 0.98.

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arXiv listing abstract v1

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Original abstract

Numerical simulations predict that the spin-down rate of a single rotation-powered neutron star depends on the angle $\alpha$ between its spin and magnetic axes as $P\dot P \propto \mu^2 (k_0 + k_1\sin^2\alpha)$, where $P$ is the star spin period, $\mu$ is its magnetic moment, while $k_0 \sim k_1 \sim 1$. Here we describe a simple observational test for this prediction based on the comparison of spin-down rates of 50 nearly orthogonal (with $\alpha$ close to 90 deg) and 27 nearly aligned (with $\alpha$ close to 0 deg) pulsars. We found, that the apparent pulsar spin-down is consistent with the theory if assumed, that magnetic moments of orthogonal rotators are systematically larger than those of aligned ones for $\sim 0.15..0.2$ dex. Also, as a by-product of the analysis, we provide yet another constraint on the average braking index of radio pulsars as $1 \le n \le 4$ with formal significance not worse than 99\%.

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