General Dimensional Theory

Sedov, L. I.

doi:10.1016/b978-1-4832-0088-0.50008-6

Cited by 212 publications

(282 citation statements)

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“…To estimate the fraction of the mass that is retained, we adopt the approach of Kashi & Soker (2011), who assumed that the released gravitational energy is instantaneously ejected at the radius r ej . Under the additional assumption of spherical symmetry, the propagation of the resulting blast wave can be followed by employing the self-similar solution of Sedov (1959). While the assumption of spherical symmetry is certainly an approximation, the calculation by Kashi & Soker (2011) indeed confirmed that the timescale for the blast wave to reach the surface of the common envelope is considerably longer than the time for the inspiral on the scale r ej , implying that the assumption of instantaneous injection is reasonable.…”

Section: Ejection Of Mass and Angular Momentummentioning

confidence: 61%

Planet formation from the ejecta of common envelopes

Schleicher

Dreizler

2014

A&A

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Context. The close binary system NN Serpentis must have gone through a common envelope phase before the formation of its white dwarf. During this phase, a substantial amount of mass was lost from the envelope. The recently detected orbits of circumbinary planets are probably inconsistent with planet formation before the mass loss. Aims. We explore whether new planets may have formed from the ejecta of the common envelope and derive the expected planetary mass as a function of radius. Methods. We employed the Kashi & Soker model to estimate the amount of mass that is retained during the ejection event and inferred the properties of the resulting disk from the conservation of mass and angular momentum. The resulting planetary masses were estimated from models with and without radiative feedback. Results. We show that the observed planetary masses can be reproduced for appropriate model parameters. Photoheating can stabilize the disks in the interior, potentially explaining the observed planetary orbits on scales of a few AU. We compare the expected mass scale of planets for 11 additional systems with observational results and find hints of two populations, one consistent with planet formation from the ejecta of common envelopes and the other a separate population that may have formed earlier.Conclusions. The formation of the observed planets from the ejecta of common envelopes seems feasible. The model proposed here can be tested through refined observations of additional post-common envelope systems. While it appears observationally challenging to distinguish between the accretion on pre-existing planets and their growth from new fragments, it may be possible to further constrain the properties of the protoplanetary disk through additional observations of current planetary candidates and post-common envelope binary systems.

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Section: Ejection Of Mass and Angular Momentummentioning

confidence: 61%

Planet formation from the ejecta of common envelopes

Schleicher

Dreizler

2014

A&A

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“…This will increase the cooling timescale of these shocks to ∼13,000 years. Assuming that the outer blast wave is moving at ∼400 km s −1 , and given that the radius of N49 is ∼7 pc, the dynamical age given by the Sedov-Taylor theory (Sedov 1959) is ∼8500 years. This value can be compared with the Sedov age of 4800 years derived from deep Chandra observations by Park et al (2012).…”

Section: Emission Line Mapsmentioning

confidence: 99%

Forbidden Iron Lines and Dust Destruction in Supernova Remnant Shocks: The Case of N49 in the Large Magellanic Cloud

Dopita

Seitenzahl

Sutherland

et al. 2016

ApJ

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We present the results of a complete integral-field survey of the bright supernova remnant (SNR) N49 in the Large Magellanic Cloud, obtained with the WiFeS instrument mounted on the ANU 2.3 m telescope at Siding Spring Observatory. From theoretical shock modeling with the new MAPPINGS 5.1 code, we have, for the first time, subjected the optical Fe emission line spectrum of an SNR to a detailed abundance and dynamical analysis covering eight separate stages of ionization. This allows us to derive the dust depletion factors as a function of ionization stage. We have shown that there is substantial (30%-90%) destruction of Fe-bearing dust grains in these fast shocks (v s ∼ 250 km s −1 ), and we have confirmed that the dominant dust destruction occurs through the nonthermal sputtering and grain-grain collision mechanisms developed in a number of theoretical works.

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“…The first efforts to model the evolution of CTB 109 were made by Hughes et al (1981) who used the Sedov-Taylor solution (Sedov 1959;Taylor 1946Taylor , 1950 to estimate the age of the remnant. For a homogeneous spherically symmetric medium they obtained an age of 17 000 yr from the Einstein data.…”

Section: Analytic Modelsmentioning

confidence: 99%

3D hydrodynamic simulations of the Galactic supernova remnant CTB 109

Bolte

Sasaki

Breitschwerdt

2015

A&A

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Context. Using detailed 3D hydrodynamic simulations we study the nature of the Galactic supernova remnant (SNR) CTB 109 (G109.1-1.0), which is well known for its semicircular shape and a bright diffuse X-ray emission feature inside the SNR. Aims. Our model has been designed to explain the observed morphology, with a special emphasis on the bright emission feature inside the SNR. Moreover, we determine the age of the remnant and compare our findings with X-ray observations. With CTB 109 we test a new method of detailed numerical simulations of diffuse young objects, using realistic initial conditions derived directly from observations. Methods. We performed numerical 3D simulations with the RAMSES code. The initial density structure has been directly taken from 12 CO emission data, adding an additional dense cloud, which, when it is shocked, causes the bright emission feature.Results. From parameter studies we obtained the position ( , b) = (109.1545 • , −1.0078 • ) for an elliptical cloud with n cloud = 25 cm −3 based on the preshock density from Chandra data and a maximum diameter of 4.54 pc, whose encounter with the supernova (SN) shock wave generates the bright X-ray emission inside the SNR. The calculated age of the remnant is about 11 000 yr according to our simulations. In addition, we can also determine the most probable site of the SN explosion. Conclusions. Hydrodynamic simulations can reproduce the morphology and the observed size of the SNR CTB 109 remarkably well. Moreover, the simulations show that it is very plausible that the bright X-ray emission inside the SNR is the result of an elliptical dense cloud shocked by the SN explosion wave. We show that numerical simulations using observational data for an initial model can produce meaningful results.

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General Dimensional Theory

Cited by 212 publications

References 0 publications

Planet formation from the ejecta of common envelopes

Planet formation from the ejecta of common envelopes

Forbidden Iron Lines and Dust Destruction in Supernova Remnant Shocks: The Case of N49 in the Large Magellanic Cloud

3D hydrodynamic simulations of the Galactic supernova remnant CTB 109

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