Radio Millisecond Pulsars

Bhattacharyya, Bhaswati; Roy, Jayanta

doi:10.1007/978-3-030-85198-9_1

Cited by 5 publications

(6 citation statements)

References 94 publications

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“…These radio pulsars have short spin periods ranging from a few to ≈ 30 milliseconds. Their period derivatives ( Ṗ ∼ 10 −18 -10 −22 ) are 3-4 orders of magnitude smaller than those of normal radio pulsars [160]. Significantly smaller period derivatives are thought to be related to much smaller dipolar magnetic fields, B ∼ 10 8 -10 10 G. MSPs are found in binaries much more frequently than normal radio pulsars.…”

Section: Millisecond Radio Pulsarsmentioning

confidence: 90%

Evolution of neutron star magnetic fields

Igoshev¹,

Попов²,

Hollerbach³

2021

Preprint

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Section: Millisecond Radio Pulsarsmentioning

confidence: 90%

Evolution of neutron star magnetic fields

Igoshev¹,

Попов²,

Hollerbach³

2021

Preprint

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“…These pulsars are the so-called MSPs. The Milky Way is estimated to host 40,000-90,000 MSPs (e.g., Bhattacharyya & Roy 2022). As the sky fraction of the zodiac belt swept by the Sun is 2π × 2θ e /(4π) ; 0.5%, the belt probably holds 200-400 MSPs.…”

Section: Mspsmentioning

confidence: 99%

Probing the Solar Interior with Lensed Gravitational Waves from Known Pulsars

Takahashi,

Morisaki,

Suyama

2023

ApJ

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When gravitational waves (GWs) from a spinning neutron star arrive from behind the Sun, they are subjected to gravitational lensing that imprints a frequency-dependent modulation on the waveform. This modulation traces the projected solar density and gravitational potential along the path as the Sun passes in front of the neutron star. We calculate how accurately the solar density profile can be extracted from the lensed GWs using a Fisher analysis. For this purpose, we selected three promising candidates (the highly spinning pulsars J1022+1001, J1730−2304, and J1745−23) from the pulsar catalog of the Australia Telescope National Facility. The lensing signature can be measured with 3σ confidence when the signal-to-noise ratio (S/N) of the GW detection reaches 100 (f/300 Hz)−1 over a 1 yr observation period (where f is the GW frequency). The solar density profile can be plotted as a function of radius when the S/N improves to ≳104.

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“…Rapidly spinning neutron stars, viz., millisecond pulsars (MSPs; spin period P < 30 ms), manifest in various incarnations [1][2][3]. The largest known population (∼500) is of radio MSPs, which show regular brightness variation at the neutron star spin period in radio wavelengths [1]. There are also more than a hundred known γ-ray MSPs, almost all of which are a subset of radio MSPs [3].…”

Section: Introductionmentioning

confidence: 99%

“…There are also more than a hundred known γ-ray MSPs, almost all of which are a subset of radio MSPs [3]. While most of these MSPs are in binary systems [1][2][3], they, with very few exceptions, do not accrete matter from the companion star [4]. These MSPs (RMSPs) are powered by neutron star spin or rotational kinetic energy [5].…”

Section: Introductionmentioning

confidence: 99%

Spin Equilibrium of Rapidly Spinning Neutron Stars via Transient Accretion

Bhattacharyya

2023

Galaxies

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The concept of spin equilibrium due to an interaction between the stellar magnetosphere and a thin, Keplerian accretion disk, and a well-known formula of the corresponding equilibrium spin frequency, provide a key understanding of spin evolution and the distribution of rapidly spinning neutron stars, viz., millisecond pulsars. However, this concept and formula are for stable accretion, but the mass transfer to most accreting millisecond pulsars is transient and the accretion rate evolves by orders of magnitude during an outburst. In this short and focussed review, we briefly discuss a relatively new concept of the spin equilibrium condition and a new formula for the equilibrium spin frequency for transiently accreting millisecond pulsars. We also review a new method to estimate this equilibrium spin frequency for observed transiently accreting millisecond pulsars, even when a pulsar has not yet attained the spin equilibrium. These will be crucial to probe the spin evolution and distribution of millisecond pulsars, and should also be applicable to all magnetic stars transiently accreting via a thin, Keplerian accretion disk.

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Radio Millisecond Pulsars

Cited by 5 publications

References 94 publications

Evolution of neutron star magnetic fields

Evolution of neutron star magnetic fields

Probing the Solar Interior with Lensed Gravitational Waves from Known Pulsars

Spin Equilibrium of Rapidly Spinning Neutron Stars via Transient Accretion

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