Dark matter: Difference between revisions
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'''Dark matter''' (DM) is aptly labeled: It is theoretical matter that can not be directly studied and observed by current technologies because it neither emits nor | '''Dark matter''' (DM) is aptly labeled: It is theoretical matter that can not be directly studied and observed by current technologies because it neither emits, absorbs, nor reflects light and appears to interact with other matter only gravitationally. As such it is presumed to exist from indirect evidence. Normal, luminous matter by contrast, composes everything commonly observed in the universe: interstellar gas and dust, galaxies, stars, planets, moons, comets, asteroids, essentially what we consider to be observable in various states. | ||
In the past few decades there has been mounting evidence that there is not enough matter in the universe to account for the amount of gravity needed to hold galaxies together. Its presence may also be inferred from the motions of astronomical objects. It would also help to explain the gravity necessary to amplify the small fluctuations in the Cosmic Microwave Background (CMB). CMB fluctuations are thought to be a reason for the large-scale structures in the universe | In the past few decades there has been mounting evidence that there is not enough matter in the universe to account for the amount of gravity needed to hold galaxies together. Its presence may also be inferred from the motions of astronomical objects. It would also help to explain the gravity necessary to amplify the small fluctuations in the Cosmic Microwave Background (CMB). CMB fluctuations are thought to be a reason for the large-scale structures in the universe | ||
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Knowing how much dark matter is present in the universe would also help to solve the questions surrounding the observed expansion of the universe and indicate its geometry. | Knowing how much dark matter is present in the universe would also help to solve the questions surrounding the observed expansion of the universe and indicate its geometry. | ||
<ref name=SchwarzString>[http://www.superstringtheory.com/cosmo/cosmo2.html What is the structure of the universe?] Schwarz, Patricia. The Official String Theory Website</ref><ref name=PreussBerkeleyLab>[http://www.lbl.gov/Science-Articles/Archive/dark-energy.html Dark energy fills the cosmos] Preuss, Paul (1999). Science Beat. The Berkeley Lab, U.S. Department of Energy.</ref><ref>[http://sci.esa.int/science-e/www/object/printfriendly.cfm?fobjectid=29097 First image and spectrum of a Dark Matter object] (2001) European Space Agency</ref><ref>[http://astro.berkeley.edu/~mwhite/darkmatter/dm.html Dark Matter] White, Martin. University of California Berkely Astronomy Dept.</ref><ref name=CalderSLAC2006>[http://home.slac.stanford.edu/pressreleases/2006/20060821.htm Dark Matter Observed: Most Direct Measurement of Dark Matter Allows Study of its Nature - Press Release] Neil Calder (August 21, 2006). Stanford Linear Accelerator Center, Stanford University, U.S. Dept of Energy</ref> | <ref name=SchwarzString>[http://www.superstringtheory.com/cosmo/cosmo2.html What is the structure of the universe?] Schwarz, Patricia. The Official String Theory Website</ref><ref name=PreussBerkeleyLab>[http://www.lbl.gov/Science-Articles/Archive/dark-energy.html Dark energy fills the cosmos] Preuss, Paul (1999). Science Beat. The Berkeley Lab, U.S. Department of Energy.</ref><ref>[http://sci.esa.int/science-e/www/object/printfriendly.cfm?fobjectid=29097 First image and spectrum of a Dark Matter object] (2001) European Space Agency</ref><ref>[http://astro.berkeley.edu/~mwhite/darkmatter/dm.html Dark Matter] White, Martin. University of California Berkely Astronomy Dept.</ref><ref name=CalderSLAC2006>[http://home.slac.stanford.edu/pressreleases/2006/20060821.htm Dark Matter Observed: Most Direct Measurement of Dark Matter Allows Study of its Nature - Press Release] Neil Calder (August 21, 2006). Stanford Linear Accelerator Center, Stanford University, U.S. Dept of Energy</ref><ref name=OstrickerSteinhardtNewLight>[http://wwwphy.princeton.edu/~steinh/osdark.pdf New Light on Dark Matter] Jeremiah P. Ostriker and Paul Steinhardt</ref> | ||
{{editintro}} | {{editintro}} | ||
==History== | ==History== | ||
Fritz Zwicky (1898-1974) was an astronomer at California | Fritz Zwicky (1898-1974) was an astronomer at California Institute of Technology. Zwicky and colleague Walter Baade were among the first to suggest that ultradense neutron stars were an evolutionary stage following supernovae,<ref>[http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1938ApJ....88..522Z&defaultprint=YES&filetype=.pdf On collapsed neutron stars] Zwicky, F. (1938) Astrophysical Journal, vol. 88, p.522-525</ref> which were in turn a source of cosmic rays.<ref>[http://www.pnas.org/cgi/reprint/20/5/259 Cosmic rays from supernovae] Baade, W. & Zwicky, F. (1934) Proceedings of the National Academy of Sciences of the United States of America, Volume 20, Issue 5, pp. 259-263 </ref> Zwicky's studies of galaxy clusters led to the observation that the velocities of galaxies within the Coma cluster were higher than predicted. At the observed velocities, it seemed reasonable that the cluster should simply have dispersed. Further data Zwicky derived from other clusters, reinforced his suspicions leading him to infer that there must be more to galaxy clusters. something he described as "an internal viscosity due to the gravitational interactions of its component masses is so high as to cause it to rotate like a solid body." He labeled this "dark matter," in a paper he published in 1933. <ref>[http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1937ApJ....86..217Z&data_type=PDF_HIGH&whole_paper=YES&type=PRINTER&filetype=.pdf On the masses of nebulae and clusters of nebulae] Zwicky, F. (1937) Astrophysicsal Journal 86:3, 217-246</ref><ref name=OstrickerSteinhardtNewLight/> | ||
Zwicky later predicted in 1937 that dark matter in sufficiently large bodies would act as gravitational lenses; when they passed between the Earth and stars, the light of the star would appear to shift position and brighten due to the gravitational effects on light. <ref>Zwicky, F. "Nebulae as Gravitational Lenses." Phys. Rev. 51, 290, 1937.</ref><ref>[http://www.slac.stanford.edu/pubs/beamline/31/1/31-1-maurer.pdf Ideaman] Maurer, Stephen (2001) Beam Line 31:1, 21-27. Stanford Linear Accelerator Center</ref> | Zwicky later predicted in 1937 that dark matter in sufficiently large bodies would act as gravitational lenses; when they passed between the Earth and stars, the light of the star would appear to shift position and brighten due to the gravitational effects on light. <ref>Zwicky, F. "Nebulae as Gravitational Lenses." Phys. Rev. 51, 290, 1937.</ref><ref>[http://www.slac.stanford.edu/pubs/beamline/31/1/31-1-maurer.pdf Ideaman] Maurer, Stephen (2001) Beam Line 31:1, 21-27. Stanford Linear Accelerator Center</ref> | ||
Vera Rubin (born 1928), an astronomer at Carnegie Institution, Washington, made further observations in the 1970s that lent credence to the theory Zwicky had proposed. While studying the nature of light (spectrograph) of galaxies, she found that contrary to Newtonian laws of gravity, stars in galaxies did not orbit as expected. Newtonian physics predicts that stars on the outside edge of a spiral galaxy would orbit slower than stars in the center of that galaxy. This is | Vera Rubin (born 1928), an astronomer at Carnegie Institution, Washington, made further observations in the 1970s that lent credence to the theory Zwicky had proposed. While studying the nature of light (spectrograph) of galaxies, she found that contrary to Newtonian laws of gravity, stars in galaxies did not orbit as expected. Newtonian physics predicts that stars on the outside edge of a spiral galaxy would orbit slower than stars in the center of that galaxy. This is similar to the way planets orbit the sun. What Vera Rubin discovered is that stars orbiting the outside of a spiral galaxy are orbiting as fast as stars near the centre. One way to explain this is that there is an invisible mass that exerts the gravity necessary to hold the galaxy in such a stable orbit pattern. Further, her work led her to posit that 90% of the universe is made of this dark matter.<ref>[http://www.sjsu.edu/depts/Museum/rubinv.html Vera Cooper Rubin] San Jose State University</ref> | ||
==Evidence to support the theory of Dark Matter== | ==Evidence to support the theory of Dark Matter== | ||
Observations | Observations in 2006 at the Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), <ref>Department of Energy’s Stanford Linear Accelerator Center (SLAC)</ref>of a galaxy cluster 3 billion light years away, have encouraged some astronomers to assert they have actually seen dark matter. | ||
{{Image|1e0657 xray labeled.jpg|left|350px|Chandra x-ray image of the two galaxy clusters in collision.}}Observers employing x-ray images of luminous matter in what has been perceived as a single “bullet cluster” have observed the collision of what is now thought to be two clusters of galaxies crossing each other at about 10 million miles per hour (approximately 16 million kilometers per hour). From x-ray images of the bullet cluster astronomers surmise that the reason for the shape is attributable to the wind produced by the high speed collison of the two clusters. | |||
These observations and accompanying analysis indicate the direct detection of independent dark matter and luminous matter. The visible luminous matter is congregated in a region separate from the invisible dark matter. | These observations and accompanying analysis indicate the direct detection of independent dark matter and luminous matter. The visible luminous matter is congregated in a region separate from the invisible dark matter. | ||
As the two galaxy clusters cross each other, the luminous matter interacts while the dark matter does not, passing through the galaxy clusters unhindered, leaving the luminous matter in its wake. The resultant separation of the two types of matter can then be studied relative to each other. | {{Image|1e0657 lens ill.jpg|right|350px|Phenomenon of gravitational lensing employed to ascertain total mass of the bullet cluster.}}As the two galaxy clusters cross each other, the luminous matter interacts while the dark matter does not, passing through the galaxy clusters unhindered, leaving the luminous matter in its wake. The resultant separation of the two types of matter can then be studied relative to each other. | ||
Detecting the separation of the two types of matter was done by comparing x-ray images of the luminous matter with the total mass of the clusters. Total mass was measured through the phenomenon of gravitational lensing. '''Gravitational lensing''' takes place when the cluster gravity distorts light from galaxies behind the clusters, the greater the distortion, the greater the mass. | Detecting the separation of the two types of matter was done by comparing x-ray images of the luminous matter with the total mass of the clusters. Total mass was measured through the phenomenon of gravitational lensing. '''Gravitational lensing''' takes place when the cluster gravity distorts light from galaxies behind the clusters, the greater the distortion, the greater the mass. | ||
These distortions were measured through the Hubble Space Telescope, the Magellan Telescopes and the Very Large Telescope. Maps of the location of the bullet cluster were compared with x-ray images of the luminous matter acquired through the Chandra X-ray Observatory, an observatory in space. These comparisons indicated four separate groups of matter, two of dark matter and two of luminous matter trailing the dark matter. | These distortions were measured through the Hubble Space Telescope, the Magellan Telescopes and the Very Large Telescope. Maps of the location of the bullet cluster were compared with x-ray images of the luminous matter acquired through the Chandra X-ray Observatory, an observatory in space. These comparisons indicated four separate groups of matter, two of dark matter and two of luminous matter trailing the dark matter. {{Image|1e0657 opt lens.jpg|right|350px|Optical image and gravitational lensing distorting the light of background stars. The mass of the luminous matter in the cluster is shown in blue. Gravitational lensing distorts the background images because of the mass in the cluster.}} | ||
The existence of the dark matter is assumed from the spatial separation while the behaviour of the two types of matter indicate their different characteristics. | The existence of the dark matter is assumed from the spatial separation while the behaviour of the two types of matter indicate their different characteristics. | ||
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Latest revision as of 16:00, 4 August 2024
Dark matter (DM) is aptly labeled: It is theoretical matter that can not be directly studied and observed by current technologies because it neither emits, absorbs, nor reflects light and appears to interact with other matter only gravitationally. As such it is presumed to exist from indirect evidence. Normal, luminous matter by contrast, composes everything commonly observed in the universe: interstellar gas and dust, galaxies, stars, planets, moons, comets, asteroids, essentially what we consider to be observable in various states.
In the past few decades there has been mounting evidence that there is not enough matter in the universe to account for the amount of gravity needed to hold galaxies together. Its presence may also be inferred from the motions of astronomical objects. It would also help to explain the gravity necessary to amplify the small fluctuations in the Cosmic Microwave Background (CMB). CMB fluctuations are thought to be a reason for the large-scale structures in the universe
These problems and their possible solution have led to the idea that there is dark matter that can not be observed directly in any known spectrum. And there seems to be a great deal of this dark matter. It appears that most of the matter in the Universe is invisible dark matter.
Dark matter would not be made of quarks as is ordinary matter: If there were enough quarks to compose dark matter then the early universe would have had to produce more helium and deuterium than could possibly exist. Possible types of DM are:
- Baryonic
- Non-Baryonic
- - hot dark matter (HDM)
- - cold dark matter (CDM),
CDM move at slower speeds and have lower pressure than HDM
Research in particle physics has led to the theory that dark matter is composed of supersymmetric particles. They are very heavy but they are weakly attracted to each other.
Knowing how much dark matter is present in the universe would also help to solve the questions surrounding the observed expansion of the universe and indicate its geometry. [1][2][3][4][5][6]
History
Fritz Zwicky (1898-1974) was an astronomer at California Institute of Technology. Zwicky and colleague Walter Baade were among the first to suggest that ultradense neutron stars were an evolutionary stage following supernovae,[7] which were in turn a source of cosmic rays.[8] Zwicky's studies of galaxy clusters led to the observation that the velocities of galaxies within the Coma cluster were higher than predicted. At the observed velocities, it seemed reasonable that the cluster should simply have dispersed. Further data Zwicky derived from other clusters, reinforced his suspicions leading him to infer that there must be more to galaxy clusters. something he described as "an internal viscosity due to the gravitational interactions of its component masses is so high as to cause it to rotate like a solid body." He labeled this "dark matter," in a paper he published in 1933. [9][6]
Zwicky later predicted in 1937 that dark matter in sufficiently large bodies would act as gravitational lenses; when they passed between the Earth and stars, the light of the star would appear to shift position and brighten due to the gravitational effects on light. [10][11]
Vera Rubin (born 1928), an astronomer at Carnegie Institution, Washington, made further observations in the 1970s that lent credence to the theory Zwicky had proposed. While studying the nature of light (spectrograph) of galaxies, she found that contrary to Newtonian laws of gravity, stars in galaxies did not orbit as expected. Newtonian physics predicts that stars on the outside edge of a spiral galaxy would orbit slower than stars in the center of that galaxy. This is similar to the way planets orbit the sun. What Vera Rubin discovered is that stars orbiting the outside of a spiral galaxy are orbiting as fast as stars near the centre. One way to explain this is that there is an invisible mass that exerts the gravity necessary to hold the galaxy in such a stable orbit pattern. Further, her work led her to posit that 90% of the universe is made of this dark matter.[12]
Evidence to support the theory of Dark Matter
Observations in 2006 at the Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), [13]of a galaxy cluster 3 billion light years away, have encouraged some astronomers to assert they have actually seen dark matter.
Observers employing x-ray images of luminous matter in what has been perceived as a single “bullet cluster” have observed the collision of what is now thought to be two clusters of galaxies crossing each other at about 10 million miles per hour (approximately 16 million kilometers per hour). From x-ray images of the bullet cluster astronomers surmise that the reason for the shape is attributable to the wind produced by the high speed collison of the two clusters.
These observations and accompanying analysis indicate the direct detection of independent dark matter and luminous matter. The visible luminous matter is congregated in a region separate from the invisible dark matter.
As the two galaxy clusters cross each other, the luminous matter interacts while the dark matter does not, passing through the galaxy clusters unhindered, leaving the luminous matter in its wake. The resultant separation of the two types of matter can then be studied relative to each other.
Detecting the separation of the two types of matter was done by comparing x-ray images of the luminous matter with the total mass of the clusters. Total mass was measured through the phenomenon of gravitational lensing. Gravitational lensing takes place when the cluster gravity distorts light from galaxies behind the clusters, the greater the distortion, the greater the mass.
These distortions were measured through the Hubble Space Telescope, the Magellan Telescopes and the Very Large Telescope. Maps of the location of the bullet cluster were compared with x-ray images of the luminous matter acquired through the Chandra X-ray Observatory, an observatory in space. These comparisons indicated four separate groups of matter, two of dark matter and two of luminous matter trailing the dark matter.
The existence of the dark matter is assumed from the spatial separation while the behaviour of the two types of matter indicate their different characteristics.
The findings from this new evidence provide a reasonable expectation that Newtonian gravity takes place on a galactic scale.
References
- ↑ What is the structure of the universe? Schwarz, Patricia. The Official String Theory Website
- ↑ Dark energy fills the cosmos Preuss, Paul (1999). Science Beat. The Berkeley Lab, U.S. Department of Energy.
- ↑ First image and spectrum of a Dark Matter object (2001) European Space Agency
- ↑ Dark Matter White, Martin. University of California Berkely Astronomy Dept.
- ↑ 5.0 5.1 Dark Matter Observed: Most Direct Measurement of Dark Matter Allows Study of its Nature - Press Release Neil Calder (August 21, 2006). Stanford Linear Accelerator Center, Stanford University, U.S. Dept of Energy
- ↑ 6.0 6.1 New Light on Dark Matter Jeremiah P. Ostriker and Paul Steinhardt
- ↑ On collapsed neutron stars Zwicky, F. (1938) Astrophysical Journal, vol. 88, p.522-525
- ↑ Cosmic rays from supernovae Baade, W. & Zwicky, F. (1934) Proceedings of the National Academy of Sciences of the United States of America, Volume 20, Issue 5, pp. 259-263
- ↑ On the masses of nebulae and clusters of nebulae Zwicky, F. (1937) Astrophysicsal Journal 86:3, 217-246
- ↑ Zwicky, F. "Nebulae as Gravitational Lenses." Phys. Rev. 51, 290, 1937.
- ↑ Ideaman Maurer, Stephen (2001) Beam Line 31:1, 21-27. Stanford Linear Accelerator Center
- ↑ Vera Cooper Rubin San Jose State University
- ↑ Department of Energy’s Stanford Linear Accelerator Center (SLAC)
- ↑ NASA Finds Direct Proof of Dark Matter NASA (Aug. 21, 2006) Marshall Space Flight Center & Chandra X-ray Center, NASA