Why do physicists think that the dark matter is cold?
$begingroup$
Most of the dark matter in the Universe is cold or nonrelativistic which rules out neutrinos as dark matter candidate as they are hot or relativistic. But why do physicists think that the dark matter is cold? How cold (i.e., how heavy) do these dark matter particles have to be?
cosmology temperature universe dark-matter
edited Dec 15 '18 at 12:41
Qmechanic♦
102k121841170
asked Dec 15 '18 at 11:23
SRSSRS
6,524432119
$endgroup$
add a comment |
$begingroup$
Most of the dark matter in the Universe is cold or nonrelativistic which rules out neutrinos as dark matter candidate as they are hot or relativistic. But why do physicists think that the dark matter is cold? How cold (i.e., how heavy) do these dark matter particles have to be?
cosmology temperature universe dark-matter
edited Dec 15 '18 at 12:41
Qmechanic♦
102k121841170
asked Dec 15 '18 at 11:23
SRSSRS
6,524432119
$endgroup$
$begingroup$
Possible duplicates: physics.stackexchange.com/q/128125/2451 and links therein.
$endgroup$
– Qmechanic♦
Dec 15 '18 at 12:40
$begingroup$
I have removed some comments that should have been posted as answers. Please use comments to ask for clarification or to suggest improvements to the question.
$endgroup$
– rob♦
Dec 15 '18 at 19:23
add a comment |
$begingroup$
Most of the dark matter in the Universe is cold or nonrelativistic which rules out neutrinos as dark matter candidate as they are hot or relativistic. But why do physicists think that the dark matter is cold? How cold (i.e., how heavy) do these dark matter particles have to be?
cosmology temperature universe dark-matter
edited Dec 15 '18 at 12:41
Qmechanic♦
102k121841170
asked Dec 15 '18 at 11:23
SRSSRS
6,524432119
$endgroup$
Most of the dark matter in the Universe is cold or nonrelativistic which rules out neutrinos as dark matter candidate as they are hot or relativistic. But why do physicists think that the dark matter is cold? How cold (i.e., how heavy) do these dark matter particles have to be?
cosmology temperature universe dark-matter
cosmology temperature universe dark-matter
edited Dec 15 '18 at 12:41
Qmechanic♦
102k121841170
asked Dec 15 '18 at 11:23
SRSSRS
6,524432119
edited Dec 15 '18 at 12:41
Qmechanic♦
102k121841170
asked Dec 15 '18 at 11:23
SRSSRS
6,524432119
edited Dec 15 '18 at 12:41
Qmechanic♦
102k121841170
edited Dec 15 '18 at 12:41
Qmechanic♦
102k121841170
edited Dec 15 '18 at 12:41
Qmechanic♦
102k121841170
102k121841170
asked Dec 15 '18 at 11:23
SRSSRS
6,524432119
asked Dec 15 '18 at 11:23
SRSSRS
6,524432119
asked Dec 15 '18 at 11:23
SRSSRS
6,524432119
6,524432119
$begingroup$
Possible duplicates: physics.stackexchange.com/q/128125/2451 and links therein.
$endgroup$
– Qmechanic♦
Dec 15 '18 at 12:40
$begingroup$
I have removed some comments that should have been posted as answers. Please use comments to ask for clarification or to suggest improvements to the question.
$endgroup$
– rob♦
Dec 15 '18 at 19:23
add a comment |
$begingroup$
Possible duplicates: physics.stackexchange.com/q/128125/2451 and links therein.
$endgroup$
– Qmechanic♦
Dec 15 '18 at 12:40
$begingroup$
I have removed some comments that should have been posted as answers. Please use comments to ask for clarification or to suggest improvements to the question.
$endgroup$
– rob♦
Dec 15 '18 at 19:23
$begingroup$
Possible duplicates: physics.stackexchange.com/q/128125/2451 and links therein.
$endgroup$
– Qmechanic♦
Dec 15 '18 at 12:40
$begingroup$
Possible duplicates: physics.stackexchange.com/q/128125/2451 and links therein.
$endgroup$
– Qmechanic♦
Dec 15 '18 at 12:40
$begingroup$
I have removed some comments that should have been posted as answers. Please use comments to ask for clarification or to suggest improvements to the question.
$endgroup$
– rob♦
Dec 15 '18 at 19:23
$begingroup$
I have removed some comments that should have been posted as answers. Please use comments to ask for clarification or to suggest improvements to the question.
$endgroup$
– rob♦
Dec 15 '18 at 19:23
add a comment |
1 Answer
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Perhaps is instructive to know why we call it cold dark matter, and why prefer it over warm or even hot dark matter. The term refers to the velocity of the particles after decoupling. It is intuitive that it is more difficult to form a gravitationally bound structure if the particles that form it move too fast. Lower thermal velocities of dark matter particles imply that structures can grow in size after they decouple from the radiation field, way before recombination. You can picture it like this:
- There are primordial seed perturbations in the density field
- If the DM particles are cold, they are slow so the these perturbations can start growing (once decoupled from expansion) even during the epoch in which baryons are still strongly coupled to radiation
- Only after recombination, baryons are able to cool down, but at that point the seed perturbations are large enough to become potential wells (dark matter halos) to baryons to settle in (dark matter halos).
Then small halos merge together to form larger ones, and so on. The result is then galaxies form smaller, and grow by mergers. This is what we call the CDM galaxy formation model.
Now compare this to a case in which DM particles are hot. Since they diffuse (Silk Damping) easier, you need larger structures as seeds. So in this picture galaxies start large, and fragment over time.
Which is one do we observe? We just need to count galaxies, turns out that CDM works best. Since dark matter halos form and grow early, baryons quickly fall into them, which results in efficient galaxy formation, efficient enough to be consistent with today's observations. Based on this you can put constraints on the mass of the dark matter particles.
For example, by counting the number of small galaxies around the Milky Way (dwarf galaxies) we can come up with a constraint on the mass of the DM. There's a problem though, small galaxies are very difficult to observe, ruling out warm dark matter has turned out to be not that easy. Well IMHO evidence points towards CDM, but you can find plenty of literature arguing in favor of WDM, here is one example.
answered Dec 15 '18 at 13:38
caveraccaverac
5,4482923
$endgroup$
$begingroup$
Wonderful answer! "_ Based on this you can put constraints on the mass of the dark matter particles._" So cold also mean that DM particles must be somewhat heavy. Any estimate how heavy? @caverac
$endgroup$
– SRS
Dec 16 '18 at 14:24
$begingroup$
@SRS That depends on the flavor of DM you prefer (there are certainly some models), e.g. SUSY has a possible candidate neutralino with as mass of around $300$ GeV, compare that with a historical candidate for hot DM, the neutrino with a mass of $0.1$ eV. I should mention that we know that neutrinos are not enough to explain structure formation, but it serves to make the point that cold particles are indeed heavier
$endgroup$
– caverac
Dec 16 '18 at 14:32
$begingroup$
Axions are also DM candidates. But have tiny masses because they are pseudo-Goldstone bosons. Can it be a candidate of CDM? @caverac
$endgroup$
– SRS
Dec 16 '18 at 14:36
$begingroup$
@SRS You are right, there's actually an experiment checking for that. But that's all I know, prefer to not say anything about it
$endgroup$
– caverac
Dec 16 '18 at 14:42
add a comment |
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$begingroup$
Perhaps is instructive to know why we call it cold dark matter, and why prefer it over warm or even hot dark matter. The term refers to the velocity of the particles after decoupling. It is intuitive that it is more difficult to form a gravitationally bound structure if the particles that form it move too fast. Lower thermal velocities of dark matter particles imply that structures can grow in size after they decouple from the radiation field, way before recombination. You can picture it like this:
- There are primordial seed perturbations in the density field
- If the DM particles are cold, they are slow so the these perturbations can start growing (once decoupled from expansion) even during the epoch in which baryons are still strongly coupled to radiation
- Only after recombination, baryons are able to cool down, but at that point the seed perturbations are large enough to become potential wells (dark matter halos) to baryons to settle in (dark matter halos).
Then small halos merge together to form larger ones, and so on. The result is then galaxies form smaller, and grow by mergers. This is what we call the CDM galaxy formation model.
Now compare this to a case in which DM particles are hot. Since they diffuse (Silk Damping) easier, you need larger structures as seeds. So in this picture galaxies start large, and fragment over time.
Which is one do we observe? We just need to count galaxies, turns out that CDM works best. Since dark matter halos form and grow early, baryons quickly fall into them, which results in efficient galaxy formation, efficient enough to be consistent with today's observations. Based on this you can put constraints on the mass of the dark matter particles.
For example, by counting the number of small galaxies around the Milky Way (dwarf galaxies) we can come up with a constraint on the mass of the DM. There's a problem though, small galaxies are very difficult to observe, ruling out warm dark matter has turned out to be not that easy. Well IMHO evidence points towards CDM, but you can find plenty of literature arguing in favor of WDM, here is one example.
answered Dec 15 '18 at 13:38
caveraccaverac
5,4482923
$endgroup$
$begingroup$
Wonderful answer! "_ Based on this you can put constraints on the mass of the dark matter particles._" So cold also mean that DM particles must be somewhat heavy. Any estimate how heavy? @caverac
$endgroup$
– SRS
Dec 16 '18 at 14:24
$begingroup$
@SRS That depends on the flavor of DM you prefer (there are certainly some models), e.g. SUSY has a possible candidate neutralino with as mass of around $300$ GeV, compare that with a historical candidate for hot DM, the neutrino with a mass of $0.1$ eV. I should mention that we know that neutrinos are not enough to explain structure formation, but it serves to make the point that cold particles are indeed heavier
$endgroup$
– caverac
Dec 16 '18 at 14:32
$begingroup$
Axions are also DM candidates. But have tiny masses because they are pseudo-Goldstone bosons. Can it be a candidate of CDM? @caverac
$endgroup$
– SRS
Dec 16 '18 at 14:36
$begingroup$
@SRS You are right, there's actually an experiment checking for that. But that's all I know, prefer to not say anything about it
$endgroup$
– caverac
Dec 16 '18 at 14:42
add a comment |
$begingroup$
Perhaps is instructive to know why we call it cold dark matter, and why prefer it over warm or even hot dark matter. The term refers to the velocity of the particles after decoupling. It is intuitive that it is more difficult to form a gravitationally bound structure if the particles that form it move too fast. Lower thermal velocities of dark matter particles imply that structures can grow in size after they decouple from the radiation field, way before recombination. You can picture it like this:
- There are primordial seed perturbations in the density field
- If the DM particles are cold, they are slow so the these perturbations can start growing (once decoupled from expansion) even during the epoch in which baryons are still strongly coupled to radiation
- Only after recombination, baryons are able to cool down, but at that point the seed perturbations are large enough to become potential wells (dark matter halos) to baryons to settle in (dark matter halos).
Then small halos merge together to form larger ones, and so on. The result is then galaxies form smaller, and grow by mergers. This is what we call the CDM galaxy formation model.
Now compare this to a case in which DM particles are hot. Since they diffuse (Silk Damping) easier, you need larger structures as seeds. So in this picture galaxies start large, and fragment over time.
Which is one do we observe? We just need to count galaxies, turns out that CDM works best. Since dark matter halos form and grow early, baryons quickly fall into them, which results in efficient galaxy formation, efficient enough to be consistent with today's observations. Based on this you can put constraints on the mass of the dark matter particles.
For example, by counting the number of small galaxies around the Milky Way (dwarf galaxies) we can come up with a constraint on the mass of the DM. There's a problem though, small galaxies are very difficult to observe, ruling out warm dark matter has turned out to be not that easy. Well IMHO evidence points towards CDM, but you can find plenty of literature arguing in favor of WDM, here is one example.
answered Dec 15 '18 at 13:38
caveraccaverac
5,4482923
$endgroup$
$begingroup$
Wonderful answer! "_ Based on this you can put constraints on the mass of the dark matter particles._" So cold also mean that DM particles must be somewhat heavy. Any estimate how heavy? @caverac
$endgroup$
– SRS
Dec 16 '18 at 14:24
$begingroup$
@SRS That depends on the flavor of DM you prefer (there are certainly some models), e.g. SUSY has a possible candidate neutralino with as mass of around $300$ GeV, compare that with a historical candidate for hot DM, the neutrino with a mass of $0.1$ eV. I should mention that we know that neutrinos are not enough to explain structure formation, but it serves to make the point that cold particles are indeed heavier
$endgroup$
– caverac
Dec 16 '18 at 14:32
$begingroup$
Axions are also DM candidates. But have tiny masses because they are pseudo-Goldstone bosons. Can it be a candidate of CDM? @caverac
$endgroup$
– SRS
Dec 16 '18 at 14:36
$begingroup$
@SRS You are right, there's actually an experiment checking for that. But that's all I know, prefer to not say anything about it
$endgroup$
– caverac
Dec 16 '18 at 14:42
add a comment |
$begingroup$
Perhaps is instructive to know why we call it cold dark matter, and why prefer it over warm or even hot dark matter. The term refers to the velocity of the particles after decoupling. It is intuitive that it is more difficult to form a gravitationally bound structure if the particles that form it move too fast. Lower thermal velocities of dark matter particles imply that structures can grow in size after they decouple from the radiation field, way before recombination. You can picture it like this:
- There are primordial seed perturbations in the density field
- If the DM particles are cold, they are slow so the these perturbations can start growing (once decoupled from expansion) even during the epoch in which baryons are still strongly coupled to radiation
- Only after recombination, baryons are able to cool down, but at that point the seed perturbations are large enough to become potential wells (dark matter halos) to baryons to settle in (dark matter halos).
Then small halos merge together to form larger ones, and so on. The result is then galaxies form smaller, and grow by mergers. This is what we call the CDM galaxy formation model.
Now compare this to a case in which DM particles are hot. Since they diffuse (Silk Damping) easier, you need larger structures as seeds. So in this picture galaxies start large, and fragment over time.
Which is one do we observe? We just need to count galaxies, turns out that CDM works best. Since dark matter halos form and grow early, baryons quickly fall into them, which results in efficient galaxy formation, efficient enough to be consistent with today's observations. Based on this you can put constraints on the mass of the dark matter particles.
For example, by counting the number of small galaxies around the Milky Way (dwarf galaxies) we can come up with a constraint on the mass of the DM. There's a problem though, small galaxies are very difficult to observe, ruling out warm dark matter has turned out to be not that easy. Well IMHO evidence points towards CDM, but you can find plenty of literature arguing in favor of WDM, here is one example.
answered Dec 15 '18 at 13:38
caveraccaverac
5,4482923
$endgroup$
Perhaps is instructive to know why we call it cold dark matter, and why prefer it over warm or even hot dark matter. The term refers to the velocity of the particles after decoupling. It is intuitive that it is more difficult to form a gravitationally bound structure if the particles that form it move too fast. Lower thermal velocities of dark matter particles imply that structures can grow in size after they decouple from the radiation field, way before recombination. You can picture it like this:
- There are primordial seed perturbations in the density field
- If the DM particles are cold, they are slow so the these perturbations can start growing (once decoupled from expansion) even during the epoch in which baryons are still strongly coupled to radiation
- Only after recombination, baryons are able to cool down, but at that point the seed perturbations are large enough to become potential wells (dark matter halos) to baryons to settle in (dark matter halos).
Then small halos merge together to form larger ones, and so on. The result is then galaxies form smaller, and grow by mergers. This is what we call the CDM galaxy formation model.
Now compare this to a case in which DM particles are hot. Since they diffuse (Silk Damping) easier, you need larger structures as seeds. So in this picture galaxies start large, and fragment over time.
Which is one do we observe? We just need to count galaxies, turns out that CDM works best. Since dark matter halos form and grow early, baryons quickly fall into them, which results in efficient galaxy formation, efficient enough to be consistent with today's observations. Based on this you can put constraints on the mass of the dark matter particles.
For example, by counting the number of small galaxies around the Milky Way (dwarf galaxies) we can come up with a constraint on the mass of the DM. There's a problem though, small galaxies are very difficult to observe, ruling out warm dark matter has turned out to be not that easy. Well IMHO evidence points towards CDM, but you can find plenty of literature arguing in favor of WDM, here is one example.
answered Dec 15 '18 at 13:38
caveraccaverac
5,4482923
answered Dec 15 '18 at 13:38
caveraccaverac
5,4482923
answered Dec 15 '18 at 13:38
caveraccaverac
5,4482923
answered Dec 15 '18 at 13:38
caveraccaverac
5,4482923
5,4482923
$begingroup$
Wonderful answer! "_ Based on this you can put constraints on the mass of the dark matter particles._" So cold also mean that DM particles must be somewhat heavy. Any estimate how heavy? @caverac
$endgroup$
– SRS
Dec 16 '18 at 14:24
$begingroup$
@SRS That depends on the flavor of DM you prefer (there are certainly some models), e.g. SUSY has a possible candidate neutralino with as mass of around $300$ GeV, compare that with a historical candidate for hot DM, the neutrino with a mass of $0.1$ eV. I should mention that we know that neutrinos are not enough to explain structure formation, but it serves to make the point that cold particles are indeed heavier
$endgroup$
– caverac
Dec 16 '18 at 14:32
$begingroup$
Axions are also DM candidates. But have tiny masses because they are pseudo-Goldstone bosons. Can it be a candidate of CDM? @caverac
$endgroup$
– SRS
Dec 16 '18 at 14:36
$begingroup$
@SRS You are right, there's actually an experiment checking for that. But that's all I know, prefer to not say anything about it
$endgroup$
– caverac
Dec 16 '18 at 14:42
add a comment |
$begingroup$
Wonderful answer! "_ Based on this you can put constraints on the mass of the dark matter particles._" So cold also mean that DM particles must be somewhat heavy. Any estimate how heavy? @caverac
$endgroup$
– SRS
Dec 16 '18 at 14:24
$begingroup$
@SRS That depends on the flavor of DM you prefer (there are certainly some models), e.g. SUSY has a possible candidate neutralino with as mass of around $300$ GeV, compare that with a historical candidate for hot DM, the neutrino with a mass of $0.1$ eV. I should mention that we know that neutrinos are not enough to explain structure formation, but it serves to make the point that cold particles are indeed heavier
$endgroup$
– caverac
Dec 16 '18 at 14:32
$begingroup$
Axions are also DM candidates. But have tiny masses because they are pseudo-Goldstone bosons. Can it be a candidate of CDM? @caverac
$endgroup$
– SRS
Dec 16 '18 at 14:36
$begingroup$
@SRS You are right, there's actually an experiment checking for that. But that's all I know, prefer to not say anything about it
$endgroup$
– caverac
Dec 16 '18 at 14:42
$begingroup$
Wonderful answer! "_ Based on this you can put constraints on the mass of the dark matter particles._" So cold also mean that DM particles must be somewhat heavy. Any estimate how heavy? @caverac
$endgroup$
– SRS
Dec 16 '18 at 14:24
$begingroup$
Wonderful answer! "_ Based on this you can put constraints on the mass of the dark matter particles._" So cold also mean that DM particles must be somewhat heavy. Any estimate how heavy? @caverac
$endgroup$
– SRS
Dec 16 '18 at 14:24
$begingroup$
@SRS That depends on the flavor of DM you prefer (there are certainly some models), e.g. SUSY has a possible candidate neutralino with as mass of around $300$ GeV, compare that with a historical candidate for hot DM, the neutrino with a mass of $0.1$ eV. I should mention that we know that neutrinos are not enough to explain structure formation, but it serves to make the point that cold particles are indeed heavier
$endgroup$
– caverac
Dec 16 '18 at 14:32
$begingroup$
@SRS That depends on the flavor of DM you prefer (there are certainly some models), e.g. SUSY has a possible candidate neutralino with as mass of around $300$ GeV, compare that with a historical candidate for hot DM, the neutrino with a mass of $0.1$ eV. I should mention that we know that neutrinos are not enough to explain structure formation, but it serves to make the point that cold particles are indeed heavier
$endgroup$
– caverac
Dec 16 '18 at 14:32
$begingroup$
Axions are also DM candidates. But have tiny masses because they are pseudo-Goldstone bosons. Can it be a candidate of CDM? @caverac
$endgroup$
– SRS
Dec 16 '18 at 14:36
$begingroup$
Axions are also DM candidates. But have tiny masses because they are pseudo-Goldstone bosons. Can it be a candidate of CDM? @caverac
$endgroup$
– SRS
Dec 16 '18 at 14:36
$begingroup$
@SRS You are right, there's actually an experiment checking for that. But that's all I know, prefer to not say anything about it
$endgroup$
– caverac
Dec 16 '18 at 14:42
$begingroup$
@SRS You are right, there's actually an experiment checking for that. But that's all I know, prefer to not say anything about it
$endgroup$
– caverac
Dec 16 '18 at 14:42
add a comment |
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Possible duplicates: physics.stackexchange.com/q/128125/2451 and links therein.
$endgroup$
– Qmechanic♦
Dec 15 '18 at 12:40
$begingroup$
I have removed some comments that should have been posted as answers. Please use comments to ask for clarification or to suggest improvements to the question.
$endgroup$
– rob♦
Dec 15 '18 at 19:23