High resolution speckle imaging of solar small-scale structure: The influence of anisoplanatism

At the boundary of a large expanding shell in Eridanus around l = 187°, b = −50° the morphology observed in the HI emission is well mimicked by the 100 μm surface brightness but with associated structures offset by as much as 0.°5. A point-to-point comparison between I100μm and NHI in filaments of neutral hydrogen and dust (IR cirrus) produces only a weak dependence. However, when I100μm at a cirrus dust peak is compared with NHI at the associated H i peak, a relationship closer to that reported by other workers is found. Preliminary CO observations have set low limits on the molecular gas in these filaments. Since the H i and dust in our region are associated with a large expanding shell (or superbubble), shocks may be responsible for separation of gas and dust. The existence of small-scale structure in both the HI and IR is noted. We conclude that attempts to correlate HI and IR must invoke high-resolution area surveys.

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Small-Scale Structure of the Mon R2 Cloud Core

International Astronomical Union Colloquium ◽

10.1017/s0252921100019734 ◽

1994 ◽

Vol 140 ◽

pp. 266-267

Author(s):

TH. Henning ◽

R. Chini ◽

W. Pfau

Keyword(s):

Star Formation ◽

High Resolution ◽

Formation Process ◽

Molecular Clouds ◽

Scale Structure ◽

Small Scale ◽

Small Scale Structure ◽

Ir Sources ◽

Cloud Core

High-resolution mm continuum observations are especially well suited to detect clumpy structures in molecular clouds. In this paper we concentrate on the Mon R2 cloud core which is associated with a cluster of IR sources. Walker et al. (1990) made a 1.3 mm map with 30″ resolution. They found an unresolved and elongated structure extending from NE to SW. Here, we discuss high-resolution continuum maps at 870 and 1300 µm showing a rich clumpy structure on the scale of several 10 arcsec. The clumps are probably intimately linked to the star formation process in Mon R2.

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A HIGH-RESOLUTION X-RAY AND OPTICAL STUDY OF SN 1006: ASYMMETRIC EXPANSION AND SMALL-SCALE STRUCTURE IN A TYPE IA SUPERNOVA REMNANT

The Astrophysical Journal ◽

10.1088/0004-637x/781/2/65 ◽

2014 ◽

Vol 781 (2) ◽

pp. 65 ◽

Cited By ~ 54

Author(s):

P. Frank Winkler ◽

Brian J. Williams ◽

Stephen P. Reynolds ◽

Robert Petre ◽

Knox S. Long ◽

...

Keyword(s):

High Resolution ◽

Supernova Remnant ◽

Scale Structure ◽

Small Scale ◽

Optical Study ◽

X Ray ◽

Small Scale Structure ◽

Type Ia Supernova ◽

Type Ia

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Small Scale Structure in the Earth's Ionosphere. Theory and Numerical Simulation.

10.21236/ada130462 ◽

1983 ◽

Author(s):

S. T. Zalesak

Keyword(s):

Numerical Simulation ◽

Scale Structure ◽

Small Scale ◽

Small Scale Structure

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A Search for Very Compact Structure in 17 OH Masers

Symposium - International Astronomical Union ◽

10.1017/s0074180900134618 ◽

1988 ◽

Vol 129 ◽

pp. 255-256

Author(s):

A. J. Kemball ◽

P. J. Diamond ◽

F. Mantovani

Keyword(s):

Galactic Disk ◽

Hii Regions ◽

Scale Structure ◽

Small Scale ◽

Compact Structure ◽

Small Scale Structure ◽

Interstellar Scattering

The apparent spot sizes of OH masers appear to be significantly broadened when seen through the inner galaxy or large extents of the galactic disk (Burke 1968). Bowers et al (1980) found evidence of small-scale structure (≲ 50 mas) in OH sources at distances of less than 5 kpc but this was characteristically absent in very distant sources (≳ 8kpc) at galactic longitudes 1 ≲ 40°. This result is typically explained in terms of interstellar scattering (ISS) by intervening diffuse HII regions.

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