Is the Sun Embedded in a Typical Interstellar Cloud?

Frisch, P. C.

doi:10.1007/s11214-008-9394-4

Cited by 15 publications

(9 citation statements)

References 68 publications

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“…In addition, Opher (2008) could show that the resulting most likely IsMF direction is also consistent with the observations by Kurth and Gurnett (2003). Frisch (2008) linked the CHISM parameters as inferred from inner heliosphere observations through detailed modeling to the wider solar neighborhood and concluded that the physical parameters are those of a warm cloud where the Sun is located close to an interface between clouds. In addition, she made the point that the currently inferred interstellar magnetic field direction is consistent with average fields obtained for the adjacent few hundred pc from Faraday rotation observations.…”

Section: Inferring the Chism From Withinsupporting

confidence: 52%

From the Heliosphere to the Local Bubble—What Have We Learned?

Möbius

2008

Space Sci Rev

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The ISSI Workshop "From the Heliosphere to the Local Bubble" has brought together space physicists who work on the in-situ study of the interaction of the heliosphere with the surrounding circum-heliospheric interstellar medium (CHISM) and astrophysicists interested in the interstellar medium itself and in the wider neighborhood known as the Local Bubble. This paper contains a summary of the workshop except for the big picture presentations given at the last day. It contains highlights as viewed by the author and is organized to lead the reader from the heliosphere, via the immediate solar neighborhood into the Local Bubble, with the attempt of a brief outlook into the future.

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Section: Inferring the Chism From Withinsupporting

confidence: 52%

From the Heliosphere to the Local Bubble—What Have We Learned?

Möbius

2008

Space Sci Rev

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“…Comparison of the widths of absorption lines of a low mass element (e.g., D) with high-mass elements (e.g., Fe and Mg) allowed to infer the gas temperature of the LIC to be T = 7500 ±1300 K and the temperatures of the other clouds to lie in the range 3900 K (Blue) to 9900 K (Mic). Frisch (2009) and Frisch, Redfield, & Slavin (2011) noted that the inferred temperatures and nonthermal broadening parameters assume a Maxwell-Boltzman distribution of velocities and mass-independent turbulence, both of which may not be valid in low density clouds. Frisch (2009) concluded that the physical properties of the CLIC clouds are typical of warm partially-ionized gas observed elsewhere in the solar neighborhood on the basis of temperature, velocity, composition, ionization, and magnetic field properties.…”

Section: Development Of Multiple Cloud Morphologiesmentioning

confidence: 99%

Evaluating the Morphology of the Local Interstellar Medium: Using New Data to Distinguish Between Multiple Discrete Clouds and a Continuous Medium

Redfield

Linsky

2015

ApJ

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Ultraviolet and optical spectra of interstellar gas along the lines of sight to nearby stars have been interpreted by and previous studies as a set of discrete warm, partially ionized clouds each with a different flow vector, temperature, and metal depletion. Recently, Gry & Jenkins (2014) have proposed a fundamentally different model consisting of a single cloud with nonrigid flows filling space out to 9 parsecs from the Sun that they propose better describes the local ISM. Here we test these fundamentally different morphological models against the spatially unbiased Malamut et al. (2014) spectroscopic data set, and find that the multiple cloud morphology model provides a better fit to both the new and old data sets. The detection of three or more velocity components along the lines of sight to many nearby stars, the presence of nearby scattering screens, the observed thin elongated structures of warm interstellar gas, and the likely presence of strong interstellar magnetic fields also support the multiple cloud model. The detection and identification of intercloud gas and the measurement of neutral hydrogen density in clouds beyond the Local Interstellar Cloud could provide future morphological tests.

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“…This model explains the results of the Dominion Radio Astrophysical Observatory Low-Resolution Polarization Survey (Wolleben et al 2006), and the model consists of two synchrotron-emitting shells, S1 and S2. The same model shell S1 was used by Frisch (2009) to explain the direction of the interstellar magnetic field at the heliosphere, the polarization of light from nearby stars, and the kinematics of nearby clouds. We studied the mutual placement of these shells and our ring, and found that the ring intersects with the shell S2 in the direction (l = 256 • , b = 43 • ) at the distance of 33 pc from the Sun.…”

Section: The Ring In Spacementioning

confidence: 99%

Gaussian decomposition of $\ion{H}{i}$ surveys

Haud¹

2010

A&A

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Context. In the previous papers of this series, we decomposed all the H i 21-cm line profiles of the Leiden-Argentina-Bonn (LAB) database into Gaussian components (GCs), and studied the statistical distributions of the obtained GCs. Aims. Now we are interested in separating the "clouds" of similar closely spaced GCs from the general database of the components. In this paper we examine the most complicated case for our new cloud-finding algorithm -the clouds of very narrow GCs. Methods. To separate the clouds of similar GCs, we started with the single-link hierarchical clustering procedure in five-dimensional (longitude, latitude, velocity, GC width, and height) space, but made some modifications to accommodate it to the large number of components. We also used the requirement that each cloud may be represented at any observed sky position by only one GC and take the similarity of global properties of the merging clouds into account. We demonstrate that the proposed algorithm enables us to find the features in gas distribution, which are described by similar GCs. As a test, we applied the algorithm for finding the clouds of the narrowest H i 21-cm line components. Results. Using the full sky search for cold clouds, we easily detected the coldest known H i clouds and demonstrate that actually they are a part of a long narrow ribbon of cold clouds. We modeled these clouds as a part of a planar gas ring, then deduce their spatial placement and discuss their relation to supernova shells in the solar neighborhood. Many other narrow-lined H i structures are also found. We conclude that the proposed algorithm satisfactorily solves the posed task. In testing the algorithm, we found a long ribbon of very cold H i clouds and demonstrated that all the observed properties of this band of clouds are described very well by the planar ring model. Conclusions.We also guess that the study of the narrowest H i 21-cm line components may be a useful tool for finding the structure of neutral gas in solar neighborhood.

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Is the Sun Embedded in a Typical Interstellar Cloud?

Cited by 15 publications

References 68 publications

From the Heliosphere to the Local Bubble—What Have We Learned?

From the Heliosphere to the Local Bubble—What Have We Learned?

Evaluating the Morphology of the Local Interstellar Medium: Using New Data to Distinguish Between Multiple Discrete Clouds and a Continuous Medium

Gaussian decomposition of $\ion{H}{i}$ surveys

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