Sputtering in interstellar shocks - A model for heavy element depletion

Barlow, M. J.; Silk, J. K.

doi:10.1086/182346

Cited by 44 publications

(25 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Ellison et al (1997, [197]) produced the first detailed model explaining GCR abundances and isotopic ratios using interstellar grains that are accelerated to modest energies by SN shock waves. Grain destruction in the shock layer results from the thermal sputtering of particles from grain surfaces due to gas-grain collisions and grain shattering and vaporization during grain-grain collisions [198,199,200,148]. Refractory elements show a well-known resilience against destruction.…”

Section: Isotopes and The Ob Association Origin Of Galactic Cosmic Raysmentioning

confidence: 99%

Effect of Supernovae on the Local Interstellar Material

Frisch¹,

Dwarkadas²

2016

Handbook of Supernovae

View full text Add to dashboard Cite

A range of astronomical data indicates that ancient supernovae created the galactic environment of the Sun and sculpted the physical properties of the interstellar medium near the heliosphere. In this paper we review the characteristics of the local interstellar medium that have been affected by supernovae. The kinematics, magnetic field, elemental abundances, and configuration of the nearest interstellar material support the view that the Sun is at the edge of the Loop I superbubble, which has merged into the low density Local Bubble. The energy source for the higher temperature X-ray emitting plasma pervading the Local Bubble is uncertain. Winds from massive stars and nearby supernovae, perhaps from the Sco-Cen Association, may have contributed radioisotopes found in the geologic record and galactic cosmic ray population. Nested supernova shells in the Orion and Sco-Cen regions suggest spatially distinct sites of episodic star formation. The heliosphere properties vary with the pressure of the surrounding interstellar cloud. A nearby supernova would modify this pressure equilibrium and thereby severely disrupt the heliosphere as well as the local interstellar medium.

show abstract

Section: Isotopes and The Ob Association Origin Of Galactic Cosmic Raysmentioning

confidence: 99%

Effect of Supernovae on the Local Interstellar Material

Frisch¹,

Dwarkadas²

2016

Handbook of Supernovae

View full text Add to dashboard Cite

show abstract

“…It was not until the detailed studies by Barlow & Silk (1977), Draine & Salpeter (1979a,b) and Cowie (1978) that a clear link was made between the enhanced gas phase abundances and the destruction of grains in low velocity shocks. Cowie (1978) shows that for clouds with velocities as low as 40−50 km s −1 the abundance of Si can be cosmic.…”

Section: Modelling Vs Observationsmentioning

confidence: 99%

Dust destruction in the ISM: a re-evaluation of dust lifetimes

Jones

Nuth

2011

A&A

201

224

View full text Add to dashboard Cite

Context. There is a long-standing conundrum in interstellar dust studies relating to the discrepancy between the time-scales for dust formation from evolved stars and the apparently more rapid destruction in supernova-generated shock waves. Aims. We re-examine some of the key issues relating to dust evolution and processing in the interstellar medium. Methods. We use recent and new constraints from observations, experiments, modelling and theory to re-evaluate dust formation in the interstellar medium (ISM). Results. We find that the discrepancy between the dust formation and destruction time-scales may not be as significant as has previously been assumed because of the very large uncertainties involved. Conclusions. The derived silicate dust lifetime could be compatible with its injection time-scale, given the inherent uncertainties in the dust lifetime calculation. The apparent need to re-form significant quantities of silicate dust in the tenuous interstellar medium may therefore not be a strong requirement. Carbonaceous matter, on the other hand, appears to be rapidly recycled in the ISM and, in contrast to silicates, there are viable mechanisms for its re-formation in the ISM.

show abstract

“…Walborn (1980), Blades (1980) and Blades & Meaburn (1980) width between Na i D and Ca ii K; the latter was stronger in the more extreme blue and red components, indicative of ionized gas or of the Routly-Spitzer effect (Routly & Spitzer 1952) explained by Barlow & Silk (1977) due to sputtering of calcium atoms off of dust grains. Both these mechanisms, ionization and sputtering are associated with hot gas.…”

Section: An Expanding Bubble Around R 136?mentioning

confidence: 99%

The VLT-FLAMES Tarantula Survey

Loon

Bailey

Tatton

et al. 2013

A&A

View full text Add to dashboard Cite

Context. The Tarantula Nebula (a.k.a. 30 Dor) is a spectacular star-forming region in the Large Magellanic Cloud (LMC), seen through gas in the Galactic disc and halo. Diffuse interstellar bands (DIBs) offer a unique probe of the diffuse, cool-warm gas in these regions. Aims. The aim is to use DIBs as diagnostics of the local interstellar conditions, whilst at the same time deriving properties of the yet-unknown carriers of these enigmatic spectral features. Methods. Spectra of over 800 early-type stars from the Very Large Telescope Flames Tarantula Survey (VFTS) were analysed. Maps were created, separately, for the Galactic and LMC absorption in the DIBs at 4428 and 6614 Å and -in a smaller region near the central cluster R 136 -neutral sodium (the Na i D doublet); we also measured the DIBs at 5780 and 5797 Å.Results. The maps show strong 4428 and 6614 Å DIBs in the quiescent cloud complex to the south of 30 Dor but weak absorption in the harsher environments to the north (bubbles) and near the OB associations. The Na maps show at least five kinematic components in the LMC and a shell-like structure surrounding R 136, and small-scale structure in the Milky Way. The strengths of the 4428, 5780, 5797 and 6614 Å DIBs are correlated, also with Na absorption and visual extinction. The strong 4428 Å DIB is present already at low Na column density but the 6614, 5780 and 5797 Å DIBs start to be detectable at subsequently larger Na column densities. Conclusions. The carriers of the 4428, 6614, 5780 and 5797 Å DIBs are increasingly prone to removal from irradiated gas. The relative strength of the 5780 and 5797 Å DIBs clearly confirm the Tarantula Nebula as well as Galactic high-latitude gas to represent a harsh radiation environment. The resilience of the 4428 Å DIB suggests its carrier is large, compact and neutral. Structure is detected in the distribution of cool-warm gas on scales between one and >100 pc in the LMC and as little as 0.01 pc in the Sun's vicinity. Stellar winds from the central cluster R 136 have created an expanding shell; some infalling gas is also detected, reminiscent of a galactic "fountain".

show abstract

Sputtering in interstellar shocks - A model for heavy element depletion

Cited by 44 publications

References 0 publications

Effect of Supernovae on the Local Interstellar Material

Effect of Supernovae on the Local Interstellar Material

Dust destruction in the ISM: a re-evaluation of dust lifetimes

The VLT-FLAMES Tarantula Survey

Contact Info

Product

Resources

About