Local Interstellar Cloud: Difference between revisions
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The cloud has a temperature of about {{convert|7000|K|-3|abbr=on}},<ref name="near-earth">{{cite web |url=https://science.nasa.gov/science-news/science-at-nasa/2003/06jan_bubble |title=Near-Earth Supernovas |publisher=NASA |series=NASA Science |date=January 6, 2003 |access-date=February 1, 2011}}</ref> about the same temperature as the surface of the Sun. However, its [[specific heat capacity]] is very low because it is not very dense, with {{convert|0.3|/cm3||sigfig=1|adj=pre|atoms}}. This is less dense than the average for the interstellar medium in the [[Milky Way]] ({{convert|0.5|/cm3||abbr=on|disp=or|sigfig=1}}), though six times denser than the gas in the hot, low-density Local Bubble ({{convert|0.05|/cm3||abbr=on|disp=or|sigfig=1}}) which surrounds the local cloud.<ref name="JPL interstellar">{{cite web |url=http://interstellar.jpl.nasa.gov/interstellar/probe/introduction/neighborhood.html |title=Our Local Galactic Neighborhood |publisher=NASA |series=Interstellar Probe Project |year=2000 |access-date=2012-08-08 |archive-url=https://web.archive.org/web/20131121061128/http://interstellar.jpl.nasa.gov/interstellar/probe/introduction/neighborhood.html |archive-date=2013-11-21 | The cloud has a temperature of about {{convert|7000|K|-3|abbr=on}},<ref name="near-earth">{{cite web |url=https://science.nasa.gov/science-news/science-at-nasa/2003/06jan_bubble |title=Near-Earth Supernovas |publisher=NASA |series=NASA Science |date=January 6, 2003 |access-date=February 1, 2011}}</ref> about the same temperature as the surface of the Sun. However, its [[specific heat capacity]] is very low because it is not very dense, with {{convert|0.3|/cm3||sigfig=1|adj=pre|atoms}}. This is less dense than the average for the interstellar medium in the [[Milky Way]] ({{convert|0.5|/cm3||abbr=on|disp=or|sigfig=1}}), though six times denser than the gas in the hot, low-density Local Bubble ({{convert|0.05|/cm3||abbr=on|disp=or|sigfig=1}}) which surrounds the local cloud.<ref name="JPL interstellar">{{cite web |url=http://interstellar.jpl.nasa.gov/interstellar/probe/introduction/neighborhood.html |title=Our Local Galactic Neighborhood |publisher=NASA |series=Interstellar Probe Project |year=2000 |access-date=2012-08-08 |archive-url=https://web.archive.org/web/20131121061128/http://interstellar.jpl.nasa.gov/interstellar/probe/introduction/neighborhood.html |archive-date=2013-11-21 }}</ref><ref name="Boulanger">{{cite conference |title=Course 7: Dust in the Interstellar Medium |book-title=Infrared Space Astronomy, Today and Tomorrow |conference=Les Houches Physics School. Grenoble, France. August 3–28, 1998. |first1=F. |last1=Boulanger |first2=P. |last2=Cox |first3=A. P. |last3=Jones |editor1-first=F. |editor1-last=Casoli|editor1-link= Fabienne Casoli |editor2-first=J. |editor2-last=Lequeux |editor3-first=F. |editor3-last=David |display-authors=1 |volume=70 |page=251 |year=2000 |bibcode=2000isat.conf..251B}}</ref> In comparison, [[Atmosphere of Earth|Earth's atmosphere]] at [[Kármán line|the edge of space]] (i.e. 100 km above sea level) has around 1.2{{e|13}} molecules per cubic centimeter, dropping to around 50 million (5.0{{e|7}}) at {{convert|450|km|mi|0|abbr=on}}.<ref>{{cite book |title=U.S. Standard Atmosphere, 1976 |publisher=[[NOAA]], [[NASA]] and [[U.S. Air Force]] |author=United States Committee on Extension to the Standard Atmosphere |pages=210–215 |date=October 1976 |oclc=3360756}}</ref> | ||
The cloud is flowing outwards from the [[Scorpius–Centaurus association]], a [[stellar association]] that is a star-forming region,<ref name="apod-1">{{Cite APOD |title=The Local Interstellar Cloud |date=February 10, 2002 |access-date=December 21, 2016}}</ref><ref name="apod-2">{{Cite APOD |title=The Local Bubble and the Galactic Neighborhood |date=February 17, 2002 |access-date=December 21, 2016}}</ref> roughly perpendicular to the Sun's own direction. | The cloud is flowing outwards from the [[Scorpius–Centaurus association]], a [[stellar association]] that is a star-forming region,<ref name="apod-1">{{Cite APOD |title=The Local Interstellar Cloud |date=February 10, 2002 |access-date=December 21, 2016}}</ref><ref name="apod-2">{{Cite APOD |title=The Local Bubble and the Galactic Neighborhood |date=February 17, 2002 |access-date=December 21, 2016}}</ref> roughly perpendicular to the Sun's own direction. | ||
Latest revision as of 14:07, 28 September 2025
Template:Short description Template:Infobox nebula
The Local Interstellar Cloud (LIC), also known as the Local Fluff, is an interstellar cloud roughly Script error: No such module "convert". across, through which the Solar System is moving. This feature overlaps with a region around the Sun referred to as the solar neighborhood.[1] It is unknown whether the Sun is embedded in the Local Interstellar Cloud, or is in the region where the Local Interstellar Cloud is interacting with the neighboring G-Cloud.[2] Like the G-Cloud and others, the LIC is part of the Very Local Interstellar Medium which begins where the heliosphere and interplanetary medium end,[3] the furthest that probes have traveled.
Structure
The Solar System is located within a structure called the Local Bubble, a low-density region of the galactic interstellar medium.[4] Within this region is the Local Interstellar Cloud (LIC), an area of slightly higher hydrogen density. It is estimated that the Solar System entered the LIC within the past 10,000 years.[5] It is uncertain whether the Sun is still inside of the LIC or has already entered a transition zone between the LIC and the G cloud.[2][5][6] A recent analysis estimates the Sun will completely exit the LIC in no more than 1,900 years.[7]
The cloud has a temperature of about Script error: No such module "convert".,[8] about the same temperature as the surface of the Sun. However, its specific heat capacity is very low because it is not very dense, with Script error: No such module "convert".. This is less dense than the average for the interstellar medium in the Milky Way (Script error: No such module "convert".), though six times denser than the gas in the hot, low-density Local Bubble (Script error: No such module "convert".) which surrounds the local cloud.[4][9] In comparison, Earth's atmosphere at the edge of space (i.e. 100 km above sea level) has around 1.2Template:E molecules per cubic centimeter, dropping to around 50 million (5.0Template:E) at Script error: No such module "convert"..[10]
The cloud is flowing outwards from the Scorpius–Centaurus association, a stellar association that is a star-forming region,[11][12] roughly perpendicular to the Sun's own direction.
In 2019, researchers found interstellar iron-60 (60Fe) in Antarctica, which they relate to the Local Interstellar Cloud.[13]
Interaction with solar magnetic field
In 2009, Voyager 2 data suggested that the magnetic strength of the local interstellar medium was much stronger than expected (370 to 550 picoteslas (pT), against previous estimates of 180 to 250 pT). The fact that the Local Interstellar Cloud is strongly magnetized could explain its continued existence despite the pressures exerted upon it by the winds that blew out the Local Bubble.[14]
The Local Interstellar Cloud's potential effects on Earth are greatly diminished by the solar wind and the Sun's magnetic field.[8] This interaction with the heliosphere is under study by the Interstellar Boundary Explorer (IBEX), a NASA satellite mapping the boundary between the Solar System and interstellar space.
See also
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- Gould Belt
- List of nearest stars and brown dwarfs
- List of nearby stellar associations and moving groups
- Orion Arm
- Perseus Arm
- Voyager program – probes left heliosphere in the 2010s
References
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- ↑ Template:Cite APOD
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Further reading
- "A Breeze from the Stars" at NASA Science
- "Voyager Makes an Interstellar Discovery" at NASA Science
- "Local Chimney and Superbubbles"
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External links
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