Ce cours vous introduit à la physique subatomique, c'est à dire à la physique du noyau et à celle des particules élémentaires. Plus spécifiquement les questions adressées sont les suivantes : - Quels sont les concepts de la physique des particules et comment sont-ils implémentés? - Quelles sont les propriétés du noyau atomique et comment peut on les utiliser? - Comment accélérer et détecter des particules et mesurer leurs propriétés? - Qu’est-ce qu’on apprend à partir des réactions de particules à haute énergie et leurs désintégrations? - Comment fonctionnent les interactions électromagnétiques et comment peut-on les mettre à contribution? - Comment fonctionnent les interactions fortes et pourquoi sont-elles difficiles à comprendre? - Comment fonctionnent les interactions faibles et pourquoi sont-elles spéciales? - Quelle est la masse des objets au niveau subatomique, et comment y intervient le Higgs? - Que peut-on apprendre de la physique des particules concernant l’astrophysique et l’Univers tout entier? Le cours est structuré en sept modules. Suivant le premier module qui introduit notre sujet, les modules 2 (Physique nucléaire) et 3 (Accélérateurs et détecteurs) dépendent peu du reste du cours et peuvent être étudiés séparément. Les modules 4 à 7 approfondissent les notions de la matière et des forces élémentaires.
7.4 Que se cache-t-il derrière la matière et l'énergie sombre ?
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En provenance du cours de University of Geneva
Physique des particules - une introduction
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À partir de la leçon
Matière et énergie sombre
Dans ce dernier module vous rencontrez la matière sombre, qui ne se manifeste que par son action gravitationnel. Vous verrez comment l'énergie sombre accélère l'expansion de notre univers. Vous apprécierez les indices observationnels qui nous démontrent l'existence de ces phénomènes mystérieuses. Et on discutera avec une spécialiste du domaine la nouvelle physique qui pourrait se cacher derrière et qui reste à découvrir.
Rencontrer les enseignants
Martin PohlProfesseur ordinaire
Département de physique nucléaire et corpusculaire
Mercedes PanicciaCollaboratrice scientifique
Département de Physique Nucléaire et Corpusculaire
[MUSIC] >> Here we are with the last video
of the last module of our introductory course on
particle physics.
And in this last video, we will go into some more depth
on the preceding discussion of dark energy and dark matter.
To do that, we have invited ourselves to a colleague from the
theoretical physics department of University of Geneva.
Let me present to you Ruth Durrer, professor of theoretical physics
who is a specialist on cosmology,
the physics subject which remains most
concerned with these two phenomena, thus far inaccessible
to experimentation at existing accelerators.
So, at the end of this video, you will understand a bit better how
dark matter and dark energy act on the universe that surrounds us.
So, Ruth,
I think there is little doubt on the existence of dark matter, is there?
Or am I mistaken, are there still people who believe that
dark matter does not exist?
>> Yes, there are such people.
Dark matter, as you have already heard in the preceding videos,
has been confirmed by only one interaction, which is gravity, and by
no other, so they ask the question: should our
theory of gravitation – to discover dark matter, one only needs
Newtonian gravitation – should it be modified at large distance scales.
There are people who have tried that, and who were able to explain, for example,
the fact that the rotational curve of galaxies does not descend
like one would expect, if gravitation obeys Kepler’s law.
But even if one can modify
gravitation such that one obtains flat rotational curves also,
there is still a lot more confirmation for the existence of dark matter.
>> Like gravitational lenses… >> Exactly.
>> …the motion of galaxies,
and their interactions, like the Bullet Cluster for example…
>> Exactly.
And if you want to explain all that by modifying the theory of gravitation,
you can for example do this with what is called TeVeS,
but it is a horribly complicated theory and one makes hypotheses which are much more
complex and non-minimal, than to just add a particle.
So, I would say that 99% of
the scientists are convinced that dark matter
is what it takes and not a modified theory of gravity.
>> And in that case, there should be a particle which constitutes
dark matter, and one should be able to see its interactions, either among themselves,
as we try with AMS, or with normal matter as out colleagues
try in Zurich, for example, in their underground experiments, or
by the artificial creation of this matter, at the LHC for example.
So, up to now, we have not succeeded to do so,
but it is never too late to try.
So, if such a particle existed,
what would be the implication for the Standard Model of
the existence of an additional particle, which we need to explain this, don’t we?
>> Of course,
such a particle is beyond the Standard Model of particle physics
but there are plenty of hypotheses on the existence of such a particle.
For example, in supersymmetry.
one expects that there be a stable supersymmetric particle.
Or one can add a heavy neutrino, to explain,
for example, the generation of quarks and leptons in the universe
and this could, at the same time, also play the role of dark matter.
A low mass neutrino does not work, because it has too large velocities
to be confined in galaxies, etc.
So, we need a particle with a minimal mass of at least
some kiloelectronvolts.
Standard candidates rather have some hundred GeV of mass.
But what is the interaction of this particle with normal matter?
Of course, we do not know.
If it is comparable to weak interactions, in the coming years
one should discover it either at LHC, or with direct or indirect
interactions. But if the interaction is much weaker,
if we had, for example a gravitino, which interacts via the
gravitational force, we will not discover it by these experiments.
>> But we are still in good hope that during our own active lifetime
we will know of what is consists.
>> Yes, I do hope so.
It is one of these problems, which are with us since 70-80 years.
>> Since Zwicky, yes.
>> Yeah. >> So, on the contrary,
I have much less hope as far as dark energy is concerned, no?
So, can you share with us your vision of dark matter.
First of all, according to you, what is it?
>> I don’t know.
This is the honest answer, we must leave somethings to do
for young people, to explain to us.
I don’t know what dark energy is.
So, I can tell you that current data are in good agreement with the
assumption, that dark energy is just a cosmological constant.
But I will talk a little about how
one has discovered the existence of this dark energy.
One has seen that the universe is currently in an accelerated expansion, and not
as one had thought, that due to gravitation the expansion would slow down more and more.
In fact, one has found that, since a while,
this slowing down has reversed and has become an acceleration.
And this acceleration,
one can explain it, if there is a component practically with negative gravity.
So, we need, for example, something which has
a very strong pressure, a negative pressure.
Negative energy density is not possible
according to the Friedmann equations
which are a consequence of the Einstein equations…
>> Well, we have scratched the surface of these equations a little bit earlier in the course,
so, if you are no more familiar with this,
please watch again the previous video, which talks just about the Friedmann equation.
So, if the famous lambda is the only thing which exists,
this would be a property of our universe, which was created together with our universe, wouldn’t it?
So, by chance, well, it has the value it has,
and we must live with it, no?
>> It is more complicated than that.
The problem is that this lambda, this cosmological constant,
must have changed, for example,
if the interactions of the universe passed through a phase transition.
>> Yes.
Like inflation, to just name one.
>> For example, during inflation.
And during that transition, the cosmological constant has changed
its value, which was 10 to the power 120
greater that the value we measure today.
So, this value requires an enormous fine tuning.
>> I.e. of the initial conditions to get there.
>> And most of all this is not what we call
a « natural » fine tuning
in the sense that in field theory
this constant is not protected from corrections.
If one modifies the theory a litle bit, this constant changes enormously, etc.
So, from the point of view of a quantum field theory,
such a constant is very, very unnatural, unexpected, bizarre.
>> So, all of this requires effectively
that his field is a quantum field, no?
Is it really necessary that this be so,
or could it not simply be a classical field,
which does not have a quantum representation, which does not exist
in a theory at small scales, does not exist or is not necessary?
>> Well, the cosmological constant itself is not a field, but it is
an effective constant, which comes from the quantisation of all other fields.
And that the electron is well represented by a quantum field,
or the quarks, I believe that you have discussed that in your course.
So you cannot say that at very small scales, this is not the case.
I would even say that usually all fields, even effective ones,
even non-fundamental ones, can be described by quantum fields,
that they exhibit a quantum nature if one talks about very small excitations.
>> Like phonons in a solid, for example.
>> Exactly, like phonons in crystals.
But here, we have two explanations, which are
a little bit more satisfactory, but more complicated and also not very attractive.
One is, one adds a scalar field,
which is not constant but nearly constant.
And with that, if the field is sufficiently constant,
one can explain dark energy.
But the difference to a cosmological constant becomes more and more
diffuse there.
Another one is that one changes the theory of gravitation at large scales.
You see, one has tested Einstein’s gravitation for distances beyond
a tenth of a millimetre,
a hundredth of a millimetre, up to the size of galaxies,
and maybe at the distance scale of the universe one must add modifications.
This can be done, there are modifications, for example concerning the graviton,
which can have a very small mass.
This mass must also be fine tuned.
But at least the quantum corrections, if one develops a quantum
theory of gravitation, are small, they are logarithmic corrections,
which do not blow up everything, when one
describes the facts by a quantum theory, like the cosmological constant does.
>> I believe that it is, however, correct to say that this form of energy is not
easily amenable to human experimentation, is it?
This is a phenomenon, which really only exists at a cosmological scale,
and which stays confined to this domain.
>> If it is a cosmological constant,
it is accessible only by gravitational forces.
All other forces are not sensitive to a constant
difference in energy.
But, if it is not a cosmological constant,
but if it is a modification, lets say, take this example,
a modification of gravity, one should be able to also see it
on other scales, with very high precision experiments, etc.
Or, if, for example, the graviton had a mass,
this would mean that the graviton has five helicities and not only two.
Ans maybe with certain experiments, still gravitational ones,
one would be able to excite these other helicities of the graviton.
So, there would be this other possibility of see that.
>> Experimental possibility.
>> Yes.
But I would say also, however,
that a cosmological experiment is a human experiment.
So, this is not to scale, but the scale
tested at LHC is as far from the human scale as the cosmological scale.
>> There, I admit, that is true.
>> You agree, Martin.
>> OK.
So, thank you very much for this interview.
I think that it is very important also
to indicate like an open window towards the future of our profession.
Because the course does not stop here.
It invites you to stay interested in the forthcoming
experimental as well as theoretical progress in the field.
So, I invite you to have eyes and ears open,
for what will happen, and for what will probably again revolutionise our field
in the coming decades.
Thank you for your attention.
[MUSIC]
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