Simulating anisotropic thermal conduction in supernova remnants – II. Implications for the interstellar medium

Balsara, Dinshaw S.; Bendinelli, Anthony J.; Tilley, David A.; Massari, Andrew R.; Howk, J. C.

doi:10.1111/j.1365-2966.2008.13121.x

Cited by 21 publications

(15 citation statements)

References 69 publications

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“…The problem of anisotropic TC in magnetized SNR has already been tackled in Tilley & Balsara (2006), Tilley et al (2006) and Balsara et al (2008a,b). As a result, the present section is intended to demonstrate the numerical method when applied to the full TC operator.…”

Section: Application To Supernova Remnants With Anisotropic Thermalmentioning

confidence: 99%

“…Thermal conduction (TC) plays an important role in transporting energy in various astrophysical systems. Its importance in regulating energy transport in supernova remnants (SNR) has been documented in various papers (Chevalier 1975; White & Long 1991; Slavin & Cox 1992, 1993, hereafter SC92 and SC93, respectively; Tilley & Balsara 2006; Tilley, Balsara & Howk 2006; Balsara, Tilley & Howk 2008a; Balsara et al 2008b). Its usefulness in shock–cloud interactions was explored in Klein, McKee & Colella (1994) and its relevance to the evolution of high‐velocity clouds was treated in Maller & Bullock (2004).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

A second-order accurate Super TimeStepping formulation for anisotropic thermal conduction

Meyer¹,

Balsara²,

Aslam³

2012

Monthly Notices of the Royal Astronomical Society

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118

109

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Astrophysical fluid dynamical problems rely on efficient numerical solution techniques for hyperbolic and parabolic terms. Efficient techniques are available for treating the hyperbolic terms. Parabolic terms, when present, can dominate the time for evaluating the solution, especially when large meshes are used. This stems from the fact that the explicit time‐step for parabolic terms is proportional to the square of the mesh size and can become unusually small when the mesh is large. Multigrid‐Newton–Krylov methods can help, but usually require a large number of iterations to converge. Super TimeStepping schemes are an interesting alternative, because they permit one to take very large overall time‐steps for the parabolic terms while using only a modest number of explicit time‐steps. Super TimeStepping schemes of the type used in astrophysics have, so far, been only first‐order accurate in time and prone to instabilities. In this paper, we present a Runge–Kutta method that is based on the recursion sequence for Legendre polynomials, called the RKL2 method. RKL2 is a time‐explicit method that permits us to treat non‐linear parabolic terms robustly and with large, second‐order accurate time‐steps. An s‐stage RKL2 scheme permits us to take a time‐step that is ∼s2 times larger than a single explicit, forward Euler time‐step for the parabolic operator. This permits an s‐fold gain in computational efficiency over explicit time‐step sub‐cycling. For modest values of ‘s’, the advantage can be substantial. The stability properties of the new schemes are explored and they are shown to be stable and positivity preserving for linear operators. We document the method as it is applied to the anisotropic thermal conduction operator for dilute, magnetized, astrophysical plasmas. Implementation‐related details are discussed. The RKL2 Super TimeStepping scheme has been implemented in the riemann code for computational astrophysics. We explain the method for picking an s‐stage RKL2 scheme for the parabolic terms and show how it can be integrated with a hyperbolic system solver. The method’s simplicity makes it very easy to retrofit the s‐stage RKL2 scheme to any problem with a parabolic part when a well‐formed spatial discretization is available. Several stringent test problems involving thermal conduction in astrophysical plasmas are presented and the method is shown to perform robustly and efficiently on all of them.

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Section: Application To Supernova Remnants With Anisotropic Thermalmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

A second-order accurate Super TimeStepping formulation for anisotropic thermal conduction

Meyer¹,

Balsara²,

Aslam³

2012

Monthly Notices of the Royal Astronomical Society

Self Cite

118

109

View full text Add to dashboard Cite

show abstract

“…What is known so far is that magnetic fields could represent a further feedback agent. In fact, current studies of magnetic fields in SN remnants suggest that they could play a role in reheating the gas at epochs of the order of a few Myr (Balsara et al 2008).…”

Section: Discussionmentioning

confidence: 99%

Feedback From Massive Stars and Gas Expulsion From Proto-Globular Clusters

Calura

Few

Romano

et al. 2015

ApJ

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Globular clusters (GCs) are considerably more complex structures than previously thought, harboring at least two stellar generations that present clearly distinct chemical abundances. Scenarios explaining the abundance patterns in GCs mostly assume that originally the clusters had to be much more massive than today, and that the second generation of stars originates from the gas shed by stars of the first generation (FG). The lack of metallicity spread in most GCs further requires that the supernova-enriched gas ejected by the FG is completely lost within ∼30 Myr, a hypothesis never tested by means of three-dimensional hydrodynamic simulations. In this paper, we use 3D hydrodynamic simulations including stellar feedback from winds and supernovae, radiative cooling and self-gravity to study whether a realistic distribution of OB associations in a massive proto-GC of initial mass M tot ∼107 M e is sufficient to expel its entire gas content. Our numerical experiment shows that the coherence of different associations plays a fundamental role: as the bubbles interact, distort, and merge, they carve narrow tunnels that reach deeper and deeper toward the innermost cluster regions, and through which the gas is able to escape. Our results indicate that after 3 Myr, the feedback from stellar winds is responsible for the removal of ∼40% of the pristine gas, and that after 14 Myr, 99% of the initial gas mass has been removed.

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“…The effective propagation velocity is very uncertain, and is expected to be in the range 100−1000 km s −1 (for example Balsara et al 2008, finds velocities of ∼200 km s −1 ). 26 Al and 60 Fe can be important for measuring this velocity, as their lifetimes are similar to the time it takes for the ejecta to cross a cavity blown by a young stellar cluster.…”

Section: Discussionmentioning

confidence: 99%

Using population synthesis of massive stars to study the interstellar medium near OB associations

Voss

Diehl²,

Hartmann

et al. 2009

A&A

127

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Aims. We study the massive stars in OB associations and their surrounding interstellar medium environment, using a population synthesis code. Methods. We developed a new population synthesis code for groups of massive stars, where we model the emission of different forms of energy and matter from the stars of the association. In particular, the ejection of the two radioactive isotopes 26 Al and 60 Fe is followed, as well as the emission of hydrogen ionizing photons, and the kinetic energy of the stellar winds and supernova explosions. We investigate various alternative astrophysical inputs and the resulting output sensitivities, especially effects due to the inclusion of rotation in stellar models. As the aim of the code is the application to relatively small populations of massive stars, special care is taken to address their statistical properties. Our code incorporates both analytical statistical methods applicable to small populations, as well as extensive Monte Carlo simulations. Results. We find that the inclusion of rotation in the stellar models has a large impact on the interactions between OB associations and their surrounding interstellar medium. The emission of 26 Al in the stellar winds is strongly enhanced, compared to non-rotating models with the same mass-loss prescription. This compensates the recent reductions in the estimates of mass-loss rates of massive stars due to the effects of clumping. Despite the lower mass-loss rates, the power of the winds is actually enhanced for rotating stellar models. The supernova power (kinetic energy of their ejecta) is decreased due to longer lifetimes of rotating stars, and therefore the wind power dominates over supernova power for the first 6 Myr after a burst of star-formation. For populations typical of nearby star-forming regions, the statistical uncertainties are large and clearly non-Gaussian.

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Simulating anisotropic thermal conduction in supernova remnants – II. Implications for the interstellar medium

Cited by 21 publications

References 69 publications

A second-order accurate Super TimeStepping formulation for anisotropic thermal conduction

A second-order accurate Super TimeStepping formulation for anisotropic thermal conduction

Feedback From Massive Stars and Gas Expulsion From Proto-Globular Clusters

Using population synthesis of massive stars to study the interstellar medium near OB associations

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