Creation of elements – supernova in the lab
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| Anzahl der Teile | 163 | |
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| Lizenz | CC-Namensnennung - keine Bearbeitung 4.0 International: Sie dürfen das Werk in unveränderter Form zu jedem legalen Zweck nutzen, vervielfältigen, verbreiten und öffentlich zugänglich machen, sofern Sie den Namen des Autors/Rechteinhabers in der von ihm festgelegten Weise nennen. | |
| Identifikatoren | 10.5446/50389 (DOI) | |
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00:00
Chemisches ElementChemisches ElementMeeresspiegelChemischer ProzessExplosion
00:24
Chemisches ElementSchussverletzungReplikationsursprung
00:30
Chemischer ProzessChemische EigenschaftBesprechung/Interview
00:35
Chemisches ElementBesprechung/Interview
00:47
Chemische EigenschaftNucleolusChemischer Prozess
00:54
Initiator <Chemie>Chemisches ElementBesprechung/Interview
01:10
NickelQuellgebietVerbrennung <Medizin>Chemischer ProzessElementanalyseChemisches ElementSchwermetallWasserstoffHydrophobe WechselwirkungValenz <Chemie>OrdnungszahlHeliumLandwirtschaftNucleolusLeiche
01:38
EisenNucleolusBindungsenergieBesprechung/Interview
01:44
QuellgebietHydrophobe WechselwirkungEisenNucleolusNickelExplosionBesprechung/Interview
02:05
Hydrophobe WechselwirkungEisenElementanalyseDeprotonierungExplosionChemisches ElementChemischer ProzessUranCobaltBukett <Wein>LeicheZeichnung
02:37
Chemische Eigenschaft
02:42
Chemische EigenschaftBiosyntheseNucleolusBesprechung/Interview
02:54
VulkanisationMagnetisierbarkeitTellerseparatorSetzen <Verfahrenstechnik>MähdrescherPegel <Hydrologie>Teilentrahmte MilchDipol <1,3->MolekularstrahlFilterChemisches Experiment
03:23
MagnetisierbarkeitVulkanisationTellerseparatorChemisches Experiment
03:29
Chemisches Experiment
03:33
VulkanisationTellerseparatorMagnetisierbarkeitNuklid
03:52
TellerseparatorSingle electron transferFilterElektronische ZigaretteChemische VerbindungenBesprechung/Interview
03:59
Elektronische ZigaretteBesprechung/Interview
04:03
Chemisches Experiment
04:07
Elektronische ZigaretteFilterBesprechung/Interview
04:12
KernproteineTankNucleolusChemisches Experiment
04:17
KernproteineBesprechung/Interview
04:28
Kernproteine
04:40
Simulation <Medizin>Konkrement <Innere Medizin>MastzelleNuklidBesprechung/Interview
04:46
Chemisches ElementSimulation <Medizin>Konkrement <Innere Medizin>
Transkript: Englisch(automatisch erzeugt)
00:06
Life on Earth is based on about 90 elements. Almost all of them were once upon a time created in the hearts of stars and during star explosions, so-called supernova. What happens in this process in stars at the microscopic level is impossible for researchers to observe.
00:24
But with the help of theoretical models and laboratory experiments, the riddles surrounding the origins of the elements can be solved, also here at the GSI in Darmstadt. My name is Caroline Selengenka, I'm a nuclear theorist and my main interest is to understand how nature produces the elements as we observe them in the universe.
00:45
This happens in stellar evolutions and as a nuclear theorist we try to simulate all the nuclear properties of those nuclei which are important in these processes. The supernova in itself, one of the most energetic events in the universe, is evolving so much
01:04
of nuclear physics, so much of exotic nuclear physics, that for theorists this is a tremendous challenge. The lighter elements are formed in the hearts of stars like our own sun. Initially, atomic cores of hydrogen fuse to form helium, the next heaviest element.
01:21
These in turn fuse to form further, even heavier elements. Thus, in heavy stars all elements of the periodic table up to iron, element 26, are formed. Then the process stops. The nuclear burning source is seized at the moment where we have reached nickel
01:42
and iron because these are the nuclei with the highest binding energy per nucleon. That means if you fuse nuclei on nickel and iron this will cost you energy and will not generate energy anymore. So this iron core then has no energy source and will then start to contract and finally collapse very fast under its own gravity.
02:01
This leads to what is called a supernova explosion. During the explosion many free neutrons are created. They then attach successively to cores which hence become very neutron rich. Thus they are very unstable and decay. In the nuclear core a neutron is transformed into a proton. This means that a different element is generated.
02:24
For example, an iron core becomes a cobalt core. Again and again neutrons are absorbed and decay. Thus within milliseconds all elements up to uranium are created. How this process unfolds exactly is what Karl-Heinz Langanker and his colleagues wish to find out.
02:43
However, if we want to simulate a supernova explosion or also the nuclear synthesis which is associated with a supernova, we have to know the properties of these nuclei. But for this we must first find them. That's like looking for a needle in a haystack. We use the super fragment separator to filter out the isotope which we
03:04
are interested in from the soup of exotic nuclear produced at the target station. The super fragment separator is a combination of superconducting dipole and quadrupole magnets where the dipole magnets are used to diverge the beam and the quadrupoles to focus it again. Here for example you see a dipole magnet which has been built by our international partners from the Butka Institute in Russia. It weighs 96 tons.
03:28
In total three such magnets are needed for the construction of the super fragment separator which will be built at the new accelerator facility FAIR. This replaces the fragment separator with which the GSI researchers have already discovered many nuclides.
03:44
A fragment separator has the ability to separate and sort the nuclides produced by the accelerator with the help of strong magnets. To filter out the isotope we are interested in, we use this particular setting at the super fragment separator. This is illustrated here with the grid size of the calendar.
04:02
If now our soup of isotopes runs through the super fragment separator, at the end with the correct setting, we filter at the end out that isotope which we want to use for the experiments. These specific nuclei can then be guided into the experimental storage ring behind us and in the storage
04:23
ring the nucleus runs by basically the speed of light several million times per second in the ring. And once it passes a certain position it gives a signal and from this signal we can determine the mass of the nucleus and we can also determine the half-life.
04:41
Karl-Heinz Lang-Anke and his colleagues can then feed the mass and half-life data of the nuclides into their theoretical models. In this way the calculations and simulations of a supernova can be made to be more and more exact. The goal? To find out how the elements of which we are made came to be.