Belgian physicist Francis Halzen, has been awarded the 2026 Nobel Prize in Physics “for decisive contributions to the IceCube Neutrino Observatory and the discovery of high-energy neutrinos of astrophysical origin.” The Royal Swedish Academy of Sciences announced the prestigious award in Stockholm on Tuesday, crediting Halzen with a central role in building the IceCube Neutrino Observatory.
This remarkable achievement recognizes Halzen’s
audacious idea to turn an enormous volume of naturally occurring Antarctic ice
into a telescope for neutrinos, providing an extraordinary window on the
universe and some of its most distant and energetic phenomena.
Halzen, a physicist at the University of Wisconsin-Madison,
first proposed what ultimately became the IceCube Neutrino Observatory in 1988.
The observatory uses thousands of light sensors buried beneath Antarctic ice to
capture ghostlike messengers known as neutrinos. These particles can travel
vast distances through space and matter, carrying information from high-energy
sources in the sky, including black holes and exploding stars. Halzen has
served as IceCube’s principal investigator since 2001, leading the decades-long
effort that transformed his ambitious idea into reality.
Together, Halzen’s vision and the discoveries made possible by
IceCube opened the world to neutrino astronomy giving scientists a
fundamentally new way to observe nature, investigate the universe’s most
energetic phenomena, and discover new questions about the cosmos
Neutrinos are tiny elementary particles with no electrical charge, but come off as byproducts of nuclear fusion reactions (see top graphic).
They're also referred to as "ghost particles:, since they rarely interact with matter.
They can travel across enormous cosmic distances almost completely undisturbed.
This allows scientists to investigate some of the universe's most energetic and
mysterious events.
However, neutrinos occasionally collide with atoms and produce
charged particles that generate faint flashes of light. These signals can be
picked up by sensitive instruments embedded deep in the clear Antarctic ice. Halzen first proposed using South Pole
ice to detect neutrinos in 1988,
An upper limit on neutrino mass published last year in the journal Science Disclosing a value of of mν < 0.45 eV at 90% confidence level, i.e.
Given effectively no mass they can cross between planets, stars and human bodies without being altered, making them rare and hard to catch. There are roughly 100 trillion solar and cosmic neutrinos that pass through our bodies every second.
At grander scales, learning more about neutrinos may help cosmologists fill in their ever hazy picture of the universe, including how galaxies originally clustered together and what influences the expansion of the cosmos since the Big Bang.
Neutrinos occur in abundance across the cosmos, created virtually anytime atomic nuclei fuse or fission. But they carry no electric charge and are notoriously difficult to detect. Neutrinos also come in three types, which physicists describe as flavors.
Let's review again the basis for these neutrino flavor states. If there are three such states: electron, muon and tau, then there must be three different corresponding neutrino masses which we can call: m1, m2 and m3. Further, the three "flavors" are really different superpositions of the 3 basic neutrino mass states. Moreover, and to make it more complex, we know that quantum interference between mass states means a neutrino originating in one "flavor" can transmogrify to another over its transit.
Because of the oscillations and quantum interference we need to reckon in a "misalignment" between flavor and the basic neutrino masses. This is done by reference to three independent "mixing angles": Θ 12 , Θ 23 and Θ 13. To a good approximation, oscillation in any one regime is characterized by just one Θ ij and a corresponding mass difference, defined:
D m ij2 = [m j2 - m i2]
Unlike the latest research published in Science, this earlier edition was confined only to mass differences ( D m) not to neutrino mass itself or even upper limits.
As an example, the probability that a muon neutrino of energy E acquires a different flavor after traversing distance L is:
P = sin2 Θ 23 sin2 (l23)
where l23 is the energy -dependent oscillation length, given by:
4ħ E c / (D m 322)
How well do we know the parameters? Atmospheric neutrino observations yield:
Θ 23 » 45 degrees, while D m 322 = 0.0024 eV2.
Meanwhile, solar neutrino data yields » 33 degrees for Θ12 and D m 212 = 0.00008 eV2. (Note: ħ is the Planck constant of action divided by 2 π) If then:
D m 312 = [D m 212 + D m 322 ] = 0.00008 eV2 + 0.0024 eV2
We know, D m 312 = 0.00248 eV2
Oddly, neutrinos can morph from one flavor to another as they move through space and time, a discovery recognized by the Nobel Prize in Physics in 2015. The underlying mechanism that makes these transformations possible, physicists realized, meant that neutrinos must have some mass. Neutrinos are mind boggingly light, and physicists don’t know why.
However, further intense research at the IceCube Neutrino Observatory may finally provide many more answers - especially for the near absence of mass.
See Also:
And:
Solar Neutrino Breakthrough: Nuclear Fusion In Sun Now Confirmed With Discovery of Solar Neutrinos
And:
AIP 2026 Nobel Prize Resources
No comments:
Post a Comment