scholarly journals Microstructure of the Local Interstellar Cloud and the Identification of the Hyades Cloud

2001 ◽  
Vol 551 (1) ◽  
pp. 413-428 ◽  
Author(s):  
Seth Redfield ◽  
Jeffrey L. Linsky
Keyword(s):  
Interstellar Cloud ◽  
Local Interstellar Cloud

The opto-mechanical design of the sub-orbital local interstellar cloud experiment (SLICE)

2013 ◽  
Author(s):  
Robert Kane ◽  
Nicholas Nell ◽  
Ted Schultz ◽  
Kevin France ◽  
Matthew Beasley ◽  
...  
Keyword(s):  
Mechanical Design ◽  
Interstellar Cloud ◽  
Local Interstellar Cloud

scholarly journals Observations of the Local Interstellar Cloud

1997 ◽  
Vol 166 ◽  
pp. 17-28
Author(s):  
R. Lallement
Keyword(s):  
Magnetic Field ◽  
Interstellar Cloud ◽  
Local Magnetic Field ◽  
Thermal Pressure ◽  
Local Bubble ◽  
Hot Gas ◽  
Local Interstellar Cloud ◽  
Nearby Stars ◽  
Local Cloud ◽  
The Magnetic Field

AbstractConstraints on the ambient (circumsolar) interstellar medium can be derived from observations of interstellar neutrals or their derivatives in the heliosphere. New results have been recently obtained which, when combined with optical and UV observations of the nearby stars (HST-GHRS, EUVE), remove long-standing contradictions and allow us to infer for our local cloud, pressure, ionization and limits on the magnetic field. The electron density in the circumsolar gas is found to be between 0.04 and 0.15 cm−3. Its total thermal pressure is within the interval 1700 – 2600 cm−3 K. If the local magnetic field is nearly perpendicular to the interstellar wind flow, which is likely, then its intensity is smaller than 3.6 μG. Our Sun is located very close to the edge of the local cloud (the volume of gas which has the same physical properties as the circumsolar gas), while there are at least 5 other cloudlets within 10 pc. Abundances vary from cloudlet to cloudlet. How they are located and whether they are separated by tenuous gas or shock discontinuities is not clear yet. Semi-hot (105 K) gas has been detected in absorption towards nearby stars (Wood et al, 1996), which probably originates in the “H walls” surrounding our heliosphere and other asterospheres. This shows that semi-hot gas is not necessarily linked with cloud interfaces with the hot gas of the Local Bubble.

scholarly journals Ultra-High Resolution Ca II Observations of the LISM

1997 ◽  
Vol 166 ◽  
pp. 37-40
Author(s):  
Barry Y. Welsh ◽  
Rosine Lallement ◽  
Ian Crawford
Keyword(s):  
High Resolution ◽  
Velocity Structure ◽  
Interstellar Cloud ◽  
Complex Velocity ◽  
Velocity Pattern ◽  
Preliminary Results ◽  
Local Interstellar Cloud ◽  
Line Absorption ◽  
The Status

AbstractWe report on the status of a long-term program of mapping the velocity structure of the local ISM using ultra-high resolution observations of Call K-line absorption towards nearby B and A-type stars. Absorption components common to the local interstellar cloud (LIC) have been detected in many (but not all) lines-of-sight. Our preliminary results indicate that the local ISM has a complex velocity pattern of inhomogeneous absorption, indicative of a shocked filamentary nature.

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