This review summarizes the observational characteristics of those interstellar grains which are prevented from entering the solar system by interactions with the heliopause. Such grains are typically less tha 100nm in radius, and they reveal their presence by interstellar absorption at ultraviolet wavelengths and by non-equilibrium emissions in the red and near-infrared portions of the spectrum
Theoretical ultraviolet extinction curves have been calculated for comparison with observed curves f...
Interstellar dust appears in a number of roles in the interstellar medium. Historically, the most fa...
Context. The size and chemical composition of interstellar dust grains are critical in setting the d...
The distribution of interstellar dust grains (ISDG) observed in the Solar System depends on the natu...
Identification by the Ulysses spacecraft of interstellar grains inside the planetary system provides...
Using ultraviolet and infrared techniques, researchers investigated the origins of the tiny (approx....
In this paper we discuss the propagation of dust through the interstellar medium (ISM), and describe...
The gas-to-dust mass ratios found for interstellar dust within the Solar System, versus values deter...
In this analysis, we illustrate how the relatively new emission mechanism, known as spinning dust, c...
Context. Theoretical predictions demonstrate that small (<0.1 μm) interstellar grains are mostly exc...
The space between the stars is filled with gas and interstellar dust (ISD). The dust grains cause ex...
No single model has been able to account for all of the observed spectroscopic properties of interst...
The typical extinction curve for the Small Magellanic Cloud (SMC), in contrast to that for the Galax...
It is shown that observed bands at 2200 A and in the 10 micron region are most probably due to colle...
We present the mass distribution of interstellar grains measured in situ by the Galileo and Ulysses ...
Theoretical ultraviolet extinction curves have been calculated for comparison with observed curves f...
Interstellar dust appears in a number of roles in the interstellar medium. Historically, the most fa...
Context. The size and chemical composition of interstellar dust grains are critical in setting the d...
The distribution of interstellar dust grains (ISDG) observed in the Solar System depends on the natu...
Identification by the Ulysses spacecraft of interstellar grains inside the planetary system provides...
Using ultraviolet and infrared techniques, researchers investigated the origins of the tiny (approx....
In this paper we discuss the propagation of dust through the interstellar medium (ISM), and describe...
The gas-to-dust mass ratios found for interstellar dust within the Solar System, versus values deter...
In this analysis, we illustrate how the relatively new emission mechanism, known as spinning dust, c...
Context. Theoretical predictions demonstrate that small (<0.1 μm) interstellar grains are mostly exc...
The space between the stars is filled with gas and interstellar dust (ISD). The dust grains cause ex...
No single model has been able to account for all of the observed spectroscopic properties of interst...
The typical extinction curve for the Small Magellanic Cloud (SMC), in contrast to that for the Galax...
It is shown that observed bands at 2200 A and in the 10 micron region are most probably due to colle...
We present the mass distribution of interstellar grains measured in situ by the Galileo and Ulysses ...
Theoretical ultraviolet extinction curves have been calculated for comparison with observed curves f...
Interstellar dust appears in a number of roles in the interstellar medium. Historically, the most fa...
Context. The size and chemical composition of interstellar dust grains are critical in setting the d...
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