Abstract
Interstellar dust and gas that enter the heliosphere provide us with important clues about both the heliosphere and the local interstellar medium (LISM). The picture we have of the LIC from both in situ detections and absorption line data presents questions that have important implications for the origins and evolution of the cloud. New detections of 60Fe on Earth in deep sea crusts and Antarctic snow cores provide evidence for the role of supernovae in shaping the LISM. We discuss our models for the evolution of the LIC inside the Local Bubble and possible explanations for the source of the supernova produced dust.
Highlights
The interstellar dust and gas that flow into the heliosphere are coming from the interstellar cloud that surrounds the Solar System known as the Local Interstellar Cloud (LIC)
That would seem to contradict the fact that the clouds have densities (n ∼ 0.2 cm−3) that are characteristic of the lower density, warm inter-cloud medium. The solution to this problem is that the clouds were dense and cold at the time they were encountered in the ISM by the first shock that carved out the Local Bubble
After being compressed by the first shocks, the clouds do rebound and at late times as the bubble pressure drops near the currently inferred values of P/kB ∼ 7000 cm−3 K, the clouds are mostly warm with temperatures near those observed for the CLIC. (More details of the simulations and results will be presented in a forthcoming paper.) we conclude that the LIC was originally cold and dense and has been subject to at least two shocks
Summary
The interstellar dust and gas that flow into the heliosphere are coming from the interstellar cloud that surrounds the Solar System known as the Local Interstellar Cloud (LIC). A knowledge of the current state of the LISM can provide important information on the history and evolution of the LISM, in particular the LIC and other nearby clouds (the Complex of Interstellar Clouds or CLIC) and the Local Bubble that surrounds the clouds.
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