Absorption of Light in the Galactic System

Trumpler, Robert J.

doi:10.1086/124039

Cited by 161 publications

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“…Trumpler (1930) studied interstellar reddening or selective absorption towards open star clusters but the effect had also, and independently, been discovered by Schalén (1929Schalén ( , 1931. However, Schalén's work on this subject in the early 1930s has largely been forgotten (Hockey et al 2014).…”

Section: Introductionmentioning

confidence: 91%

“…Indeed, Schalén (1934) and Schoenberg & Jung (1934) used Gustave Mie's theory (Mie 1908) to study the diffusion of starlight by interstellar matter and found that the interstellar absorption could be reproduced by metallic particles. Sometime later followed the so-called "dirty ice" model proposed by van de Hulst (1943), which was further developed by Oort & van de Hulst (1946). In the latter work Oort and van de Hulst determined that accretion in the interstellar medium (ISM) on a time-scale 10 8 yr would form grains with radii of 100 nm.…”

Section: Introductionmentioning

confidence: 99%

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The global dust modelling framework THEMIS

Jones

Koehler

Ysard

et al. 2017

A&A

256

345

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Here we introduce the interstellar dust modelling framework THEMIS (The Heterogeneous dust Evolution Model for Interstellar Solids), which takes a global view of dust and its evolution in response to the local conditions in interstellar media. This approach is built upon a core model that was developed to explain the dust extinction and emission in the diffuse interstellar medium. The model was then further developed to self-consistently include the effects of dust evolution in the transition to denser regions. The THEMIS approach is under continuous development and we are currently extending the framework to explore the implications of dust evolution in HII regions and the photon-dominated regions associated with star formation. We provide links to the THEMIS, DustEM and DustPedia websites where more information about the model, its input data and applications can be found.

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Section: Introductionmentioning

confidence: 91%

Section: Introductionmentioning

confidence: 99%

The global dust modelling framework THEMIS

Jones

Koehler

Ysard

et al. 2017

A&A

256

345

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“…In 1930 the attenuation of starlight over kpc galactic distances was recognized as caused by interstellar dust (Trumpler 1930). This wavelength-dependent attenuation -"extinction" of distant stars from UV to infrared wavelengths -has provided us with knowledge of the interstellar dust size distribution, and spectral absorption features have revealed its chemical composition.…”

Section: Introductionmentioning

confidence: 99%

The filtering of interstellar dust in the solar system

Sterken

Altobelli

Kempf

et al. 2013

A&A

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Context. Theoretical predictions demonstrate that small (<0.1 µm) interstellar grains are mostly excluded from reaching the planetary system by electromagnetic interactions in the heliopause region and in the inner heliosphere. Bigger interstellar grains have been recorded in the planetary system by dust measurements on board Ulysses and other spacecraft. It was found that the interstellar dust flux is modulated by the interplanetary magnetic field. Aims. The objective of this study is to analyze the heliospheric filtering of the interstellar dust flow through the solar system and throughout the solar cycle. In the heliosphere the dynamics of interstellar dust is governed by the gravitational pull of the Sun, by the repulsion of solar radiation, and by the deflection caused by the interaction of the charged interstellar dust (ISD) grains with the interplanetary magnetic field. These interactions are described by the parameters of the radiation pressure constant β and the charge-to-mass ratio Q/m, which depend on the particle's size, physical properties, and composition. A previous paper studied the flow characteristics of ISD moving through the solar system were studied. In this follow-up paper, we focus on how the ISD size distribution varies during its passage through the solar system. Methods. In a parametric study of 70 different β and Q/m values, we calculated interstellar dust trajectories starting at the boundary of the heliosphere with starting times spread over a complete solar cycle of 22 years. Results. As a result we obtained the interstellar dust flux and dust speed for these times and positions and demonstrate the effects of the filtering on the dust size distributions. The size distribution of ISD observed at any time and at any position in the planetary system is strongly modified from when it entered the heliosphere. Peaks in relative flux of 10 times the original flux possibly depend on the grain size and place and time in the solar system. We did a detailed study of three cases of the flux and size distribution of interstellar grains reaching the planets Saturn, Jupiter, and the main-belt asteroid Ceres. These cases are used to get a first idea of what a dust detector or collector on a mission to these bodies might see of ISD.

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“…In particular, this dust coagulates into larger "dust balls" and eventually cometesimals and planetesimals in the disks around young stellar objects in the first steps towards the formation of a new planetary system. It is clear that many of the key processes in the interstellar medium involve dust and, conversely, that the characteristics and physical properties of dust are key to our understanding of the Universe.The presence of interstellar dust grains was first surmised from their extinction effects on starlight (Trumpler 1930), and for much of the last century most of our information on interstellar dust was derived from extinction studies supplemented by a smither of scattering and polarization data. Really what this data probed was the size distribution of interstellar dust and during the sixties and seventies -thanks to the opening up of the UV window by space-based observations -these studies culminated in the influential Mathis et al (1977) dust model with steep (index -3.5) powerlaw grain size distributions ranging from 100 Å to 3000 Å.…”

mentioning

confidence: 99%

“…The presence of interstellar dust grains was first surmised from their extinction effects on starlight (Trumpler 1930), and for much of the last century most of our information on interstellar dust was derived from extinction studies supplemented by a smither of scattering and polarization data. Really what this data probed was the size distribution of interstellar dust and during the sixties and seventies -thanks to the opening up of the UV window by space-based observations -these studies culminated in the influential Mathis et al (1977) dust model with steep (index -3.5) powerlaw grain size distributions ranging from 100 Å to 3000 Å.…”

mentioning

confidence: 99%

The large and the small of interstellar dust

Tielens

2009

A&A

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Dust is an important component of the interstellar medium of galaxies. Dust dominates the extinction, hence also radiative transfer, of non-ionizing radiation and therefore the optical to sub-millimeter appearance of galaxies. The high dust extinction for energetic UV photons -associated with molecular cloudsalso allows molecules to survive. Moreover, grain surfaces provide a catalytic agent for the drive towards molecular complexity in these environments. Small grains also play a major role in the energy balance of interstellar gas through the photoelectric effect, so they control the phase structure of the interstellar medium. Eventually, these small dust grains partake in the process of star and planet formation. In particular, this dust coagulates into larger "dust balls" and eventually cometesimals and planetesimals in the disks around young stellar objects in the first steps towards the formation of a new planetary system. It is clear that many of the key processes in the interstellar medium involve dust and, conversely, that the characteristics and physical properties of dust are key to our understanding of the Universe.The presence of interstellar dust grains was first surmised from their extinction effects on starlight (Trumpler 1930), and for much of the last century most of our information on interstellar dust was derived from extinction studies supplemented by a smither of scattering and polarization data. Really what this data probed was the size distribution of interstellar dust and during the sixties and seventies -thanks to the opening up of the UV window by space-based observations -these studies culminated in the influential Mathis et al. (1977) dust model with steep (index -3.5) powerlaw grain size distributions ranging from 100 Å to 3000 Å. The field sort of stagnated at this point. Admittedly, at about any astronomical meeting in the next decade, there was much discussion on the composition, origin, and evolution of interstellar dust -aspects that were not wellconstrained by the observations -but that was mainly driven by the force of personalities rather than by new developments.In hindsight, this started to change dramatically in the late seventies, driven by the advent of infrared detector technology, which in many ways provided a new view of the dusty Universe. Some of this reflected the rise of infrared absorption spectroscopy as a very powerful way of probing the composition of solid compounds. Studies of infrared emission spectra, though, provided a much more dramatic revolution in our understanding of interstellar dust. In particular, airborne observations revealed that broad emission features dominate the mid-infrared spectra of many luminous objects. Subsequently, observations with the InfraRed Astronomical Satellite showed that widespread mid-infrared emission is a general characteristic of the diffuse interstellar medium. In a seminal paper in the mideighties, Kris Sellgren (1984) observed mid-infrared emission far from the illuminating stars in reflection nebulae and realized th...

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Absorption of Light in the Galactic System

Cited by 161 publications

References 0 publications

The global dust modelling framework THEMIS

The global dust modelling framework THEMIS

The filtering of interstellar dust in the solar system

The large and the small of interstellar dust

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