Dynamics of the clumps partially disrupted from a planet around a neutron star

Kurban, Abdusattar; Xia, Zhou; Wang, Na; Huang, Yong-Feng; Wang, Yubin; Nurmamat, Nurimangul

doi:10.1093/mnras/stad1260

Cited by 4 publications

(2 citation statements)

References 88 publications

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“…are the semimajor axis and eccentricity of the clump, respectively [31]. Then the clumps' periastron distance is R cl P 5.67 × 10 10 cm.…”

Section: Comparison With Frb 180916mentioning

confidence: 99%

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Repeating fast radio bursts produced by a strange star interacting with its planet in an eccentric orbit

Nurmamat,

Huang,

Geng

et al. 2024

Eur. Phys. J. C

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FRB 180916 is an important repeating fast radio burst (FRB) source. Interestingly, the activity of FRB 180916 shows a well-regulated behavior, with a period of 16.35 days. The bursts are found to occur in a duty cycle of about 5 days in each period. In this study, we suggest that the bursts of FRB 180916 are produced by a strange star interacting with its planet. The planet moves in a highly eccentric orbit around its compact host, with the periastron only slightly beyond the tidal disruption radius. As a result, the planet will be partially disrupted every time it passes through the periastron. The stripped material from the planet will be accreted by the strange star, falling to the polar cap region along the magnetic field lines and accumulated there. It will finally lead to a local collapse when the crust at the polar region is overloaded, triggering an FRB. The observed 16.35 day period corresponds to the orbital motion of the planet, and the 5 day duty cycle is explained as the duration of the partial disruption near the periastron. The energy released in each local collapse event can be as high as $$\sim 10^{42}\,\textrm{erg}$$ ∼ 10 42 erg , which is large enough to account for typical FRBs even if the radiation efficiency is low.

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“…are the semimajor axis and eccentricity of the clump, respectively [31]. Then the clumps' periastron distance is R cl P 5.67 × 10 10 cm.…”

Section: Comparison With Frb 180916mentioning

confidence: 99%

“…However, they will also be completely disrupted by the tidal force when their distance to the SS is ∼ 10 9 cm. Thus they will still fall toward the polar regions along the magnetic field lines [31].…”

Section: Introductionmentioning

confidence: 99%

Repeating fast radio bursts produced by a strange star interacting with its planet in an eccentric orbit

Nurmamat,

Huang,

Geng

et al. 2024

Eur. Phys. J. C

Self Cite

View full text Add to dashboard Cite

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Repeating X-ray bursts: Interaction between a neutron star and clumps partially disrupted from a planet

Kurban,

Zhou,

Wang

et al. 2024

A&A

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Repeating X-ray bursts from the Galactic magnetar SGR 1806-20 have been observed with a period of 398 days. Similarly, periodic X-ray bursts from SGR 1935+2154 with a period of 238 days have also been observed. Here we argue that these X-ray bursts could be produced by the interaction of a neutron star (NS) with its planet in a highly elliptical orbit. The periastron of the planet is very close to the NS, so it would be partially disrupted by the tidal force every time it passes through the periastron. Major fragments generated in the process will fall onto the NS under the influence of gravitational perturbation. The collision of the in-falling fragments with the NS produces repeating X-ray bursts. The main features of the observed X-ray bursts, such as their energy, duration, periodicity, and activity window, can all be explained in our framework.

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Probing the eccentricity in protostellar discs: Modelling kinematics and morphologies

Ragusa,

Lynch,

Laibe

et al. 2024

A&A

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Protostellar discs are mostly modelled as circular structures of gas and dust orbiting a protostar. However, a number of physical mechanisms, for example, the presence of a (sub)stellar companion or initial axial asymmetry, can cause the gas and dust orbital motion to become eccentric. Theoretical studies have revealed that, when present, disc eccentricity is expected to occur with predictable profiles that can be long-lasting and potentially observable in protostellar systems. We construct an analytical model predicting the typical features of the kinematics and morphology of eccentric protostellar discs, with the final goal of characterising the observational appearance of eccentricity in discs. We validate the model using a numerical simulation of a circumbinary disc (where the binary makes the disc eccentric). We finally post-process the simulation with Monte Carlo radiative transfer to study how eccentric features would appear through the 'eyes' of ALMA. Besides the motion of the material on eccentric Keplerian orbits in the disc orbital plane, the most characteristic eccentric feature emerging from the analytical model is strong vertical motion with a typical anti-symmetric pattern (with respect to the disc line of pericentres). A circumbinary disc with a $ 40$ au eccentric cavity cav =0.2$), carved by an $a_ bin =15$ au binary, placed at a distance $d=130$ pc, is expected to host in its upper emission surface vertical oscillations up to $v_ z ms $ close to the cavity edge, that is to say, well within ALMA spectral and spatial resolution capabilities. A residual spiral pattern in the vertical velocity $ z ms $ of the simulation cannot be captured by the theoretical model, we speculate it to be possibly linked to the presence of a companion in the system.

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Dynamics of the clumps partially disrupted from a planet around a neutron star

Cited by 4 publications

References 88 publications

Repeating fast radio bursts produced by a strange star interacting with its planet in an eccentric orbit

Repeating fast radio bursts produced by a strange star interacting with its planet in an eccentric orbit

Repeating X-ray bursts: Interaction between a neutron star and clumps partially disrupted from a planet

Probing the eccentricity in protostellar discs: Modelling kinematics and morphologies

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