2011MNRAS.414.2069T

Query : 2011MNRAS.414.2069T

2011MNRAS.414.2069T - Mon. Not. R. Astron. Soc., 414, 2069-2086 (2011/July-1)

Relativistic expansion of magnetic loops at the self-similar stage – II. Magnetized outflows interacting with the ambient plasma.

TAKAHASHI H.R., ASANO E. and MATSUMOTO R.

Abstract (from CDS):

We obtained self-similar solutions of relativistically expanding magnetic loops by assuming axisymmetry and a purely radial flow. The stellar rotation and the magnetic fields in the ambient plasma are neglected. We include the Newtonian gravity of the central star. These solutions are extended from those in our previous work by taking into account discontinuities such as the contact discontinuity and the shock. The global plasma flow consists of three regions, the outflowing region, the post-shocked region and the ambient plasma. They are divided by two discontinuities. The solutions are characterized by the radial velocity, which plays a role of the self-similar parameter in our solutions. The shock Lorentz factor gradually increases with radius. It can be approximately represented by the power of radius with the power-law index of 0.25.

We also carried out magnetohydrodynamic (MHD) simulations of the evolution of magnetic loops to study the stability and the generality of our analytical solutions. We used the analytical solutions as the initial condition and the inner boundary conditions. We confirmed that our solutions are stable over the simulation time and that numerical results nicely recover the analytical solutions. We then carried out numerical simulations to study the generality of our solutions by changing the power-law index δ of the ambient plasma density ρ₀∝r^–δ. We alter the power-law index δ from δ ≃ 3.5 in the analytical solutions. The analytical solutions are used as the initial conditions inside the shock in all simulations. We observed that the shock Lorentz factor increases with time when the power-law index is larger than 3, while it decreases with time when the power-law index is smaller than 3. The shock Lorentz factor Γ_s can be expressed as Γ_s∝t^(δ–3)/2 where δ is the power-law index of the ambient plasma. These results are consistent with the analytical studies by Shapiro.

Abstract Copyright: 2011 The Authors Monthly Notices of the Royal Astronomical Society2011 RAS

Journal keyword(s): hydrodynamics - magnetic fields - stars: flare - stars: magnetic fields - stars: neutron

Simbad objects: 1

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Number of rows : 1

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag U	Mag B	Mag V	Mag R	Mag I	Sp type	#ref 1850 - 2026	#notes
1	PSR J1808-2024	Psr	18 08 39.32	-20 24 40.1						~	1316	2

Query : 2011MNRAS.414.2069T

Basic data :

PSR J1808-2024 -- Pulsar
Other object types:	`X (2022MNRAS,AX,...)`, `gB (GBS,GRB,...)`, `Psr (2012ApJ,PSR)`, `gam (INTEGRAL1,INTREF)`, `Rad (MITG)`, `IR ([FMC99])`
ICRS coord. (ep=J2000) :	`18 08 39.32 -20 24 40.1 (X-ray) [ 100 100 90 ] C 2012ApJ...756...27L`
FK4 coord. (ep=B1950 eq=1950) :	`18 05 40.68 -20 25 11.4 [ 100 100 90 ]`
Gal coord. (ep=J2000) :	`009.99584 -00.24194 [ 100 100 90 ]`

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`PSR J1808-2024`	`GRB 041227`	`KONUS 07.01.79`	`SWIFT J1808.6-2024`
`AX 1805.7-2025`	`HETE Trigger 3800`	`MITG J1808-2024`	`2XMM J180839.2-202439`
`CXOU J180839.3-202439`	`HETE Trigger 3801`	`NAME Sgr 1806-20`	`[ABH87] 25`
`GBS 1806-20`	`HETE Trigger 1566`	`PBC J1808.5-2025`	`[FMC99] O`
`GRB 970912`	`INTEGRAL1 84`	`RX J1808.6-2024`	`[KRL2007b] 305`
`GRB 790107`	`INTREF 882`	`SWIFT J1808.7-2024`	`EQ 1805.7-2025`

References (1316 between 1850 and 2026) (Total 1316)
Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system).

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Data at NED - NASA/IPAC Extragalactic Database : PSR J1808-2024

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MITG J1808-2024

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