Simulated Large Hadron ColliderCMS particle detector data depicting a Higgs boson produced by colliding protons decaying into hadron jets and electrons
Neutrino oscillation is a quantum mechanical phenomenon in which a neutrino created with a specific leptonfamily number ("lepton flavor": electron, muon, or tau) can later be measured to have a different lepton family number. The probability of measuring a particular flavor for a neutrino varies between three known states, as it propagates through space.[1]
First predicted by Bruno Pontecorvo in 1957,[2][3] neutrino oscillation has since been observed by a multitude of experiments in several different contexts. Most notably, the existence of neutrino oscillation resolved the long-standing solar neutrino problem.
A great deal of evidence for neutrino oscillation has been collected from many sources, over a wide range of neutrino energies and with many different detector technologies.[7] The 2015 Nobel Prize in Physics was shared by Takaaki Kajita and Arthur B. McDonald for their early pioneering observations of these oscillations.
Neutrino oscillation is a function of the ratio L / E , where L is the distance traveled and E is the neutrino's energy. (Details in § Propagation and interference below.) All available neutrino sources produce a range of energies, and oscillation is measured at a fixed distance for neutrinos of varying energy. The limiting factor in measurements is the accuracy with which the energy of each observed neutrino can be measured. Because current detectors have energy uncertainties of a few percent, it is satisfactory to know the distance to within 1%.
Solar neutrino oscillation
The first experiment that detected the effects of neutrino oscillation was Ray Davis'Homestake experiment in the late 1960s, in which he observed a deficit in the flux of solar neutrinos with respect to the prediction of the Standard Solar Model, using a chlorine-based detector.[8] This gave rise to the solar neutrino problem. Many subsequent radiochemical and water Cherenkov detectors confirmed the deficit, but neutrino oscillation was not conclusively identified as the source of the deficit until the Sudbury Neutrino Observatory provided clear evidence of neutrino flavor change in 2001.[9]
Solar neutrinos have energies below 20 MeV. At energies above 5 MeV, solar neutrino oscillation actually takes place in the Sun through a resonance known as the MSW effect, a different process from the vacuum oscillation described later in this article.[1]
Atmospheric neutrino oscillation
Following the theories that were proposed in the 1970s suggesting unification of electromagnetic, weak, and strong forces, a few experiments on proton decay followed in the 1980s. Large detectors such as IMB, MACRO, and Kamiokande II have observed a deficit in the ratio of the flux of muon to electron flavor atmospheric neutrinos (see muon decay). The Super-Kamiokande experiment provided a very precise measurement of neutrino oscillation in an energy range of hundreds of MeV to a few TeV, and with a baseline of the diameter of the Earth; the first experimental evidence for atmospheric neutrino oscillations was announced in 1998.[10]
Reactor neutrino oscillation
Many experiments have searched for oscillation of electron anti-neutrinos produced in nuclear reactors. No oscillations were found until a detector was installed at a distance 1–2 km. Such oscillations give the value of the parameter θ13. Neutrinos produced in nuclear reactors have energies similar to solar neutrinos, of around a few MeV. The baselines of these experiments have ranged from tens of meters to over 100 km (parameter θ12). Mikaelyan and Sinev proposed to use two identical detectors to cancel systematic uncertainties in reactor experiment to measure the parameter θ13.[11]
In December 2011, the Double Chooz experiment found thatθ13 ≠ 0 .[12] Then, in 2012, the Daya Bay experiment found thatθ13 ≠ 0 with a significance of 5.2 σ ;[13] These results have since been confirmed by RENO.[14]
Beam neutrino oscillation
Neutrino beams produced at a particle accelerator offer the greatest control over the neutrinos being studied. Many experiments have taken place that study the same oscillations as in atmospheric neutrino oscillation using neutrinos with a few GeV of energy and several-hundred-km baselines. The MINOS, K2K, and Super-K experiments have all independently observed muon neutrino disappearance over such long baselines.[1]
Data from the LSND experiment appear to be in conflict with the oscillation parameters measured in other experiments. Results from the MiniBooNE appeared in Spring 2007 and contradicted the results from LSND, although they could support the existence of a fourth neutrino type, the sterile neutrino.[1]
T2K, using a neutrino beam directed through 295 km of earth and the Super-Kamiokande detector, measured a non-zero value for the parameter θ13 in a neutrino beam.[16]NOνA, using the same beam as MINOS with a baseline of 810 km, is sensitive to the same.
Theory
Neutrino oscillation arises from mixing between the flavor and mass eigenstates of neutrinos. That is, the three neutrino states that interact with the charged leptons in weak interactions are each a different superposition of the three (propagating) neutrino states of definite mass. Neutrinos are emitted and absorbed in weak processes in flavor eigenstates[a] but travel as mass eigenstates.[18]
As a neutrino superposition propagates through space, the quantum mechanical phases of the three neutrino mass states advance at slightly different rates, due to the slight differences in their respective masses. This results in a changing superposition mixture of mass eigenstates as the neutrino travels; but a different mixture of mass eigenstates corresponds to a different mixture of flavor states. For example, a neutrino born as an electron neutrino will be some mixture of electron, mu, and tau neutrino after traveling some distance. Since the quantum mechanical phase advances in a periodic fashion, after some distance the state will nearly return to the original mixture, and the neutrino will be again mostly electron neutrino. The electron flavor content of the neutrino will then continue to oscillate – as long as the quantum mechanical state maintains coherence. Since mass differences between neutrino flavors are small in comparison with long coherence lengths for neutrino oscillations, this microscopic quantum effect becomes observable over macroscopic distances.
In contrast, due to their larger masses, the charged leptons (electrons, muons, and tau leptons) have never been observed to oscillate. In nuclear beta decay, muon decay, pion decay, and kaon decay, when a neutrino and a charged lepton are emitted, the charged lepton is emitted in incoherent mass eigenstates such as | e− ⟩ , because of its large mass. Weak-force couplings compel the simultaneously emitted neutrino to be in a "charged-lepton-centric" superposition such as | ν e ⟩ , which is an eigenstate for a "flavor" that is fixed by the electron's mass eigenstate, and not in one of the neutrino's own mass eigenstates. Because the neutrino is in a coherent superposition that is not a mass eigenstate, the mixture that makes up that superposition oscillates significantly as it travels. No analogous mechanism exists in the Standard Model that would make charged leptons detectably oscillate. In the four decays mentioned above, where the charged lepton is emitted in a unique mass eigenstate, the charged lepton will not oscillate, as single mass eigenstates propagate without oscillation.
The case of (real) W boson decay is more complicated: W boson decay is sufficiently energetic to generate a charged lepton that is not in a mass eigenstate; however, the charged lepton would lose coherence, if it had any, over interatomic distances (0.1 nm) and would thus quickly cease any meaningful oscillation. More importantly, no mechanism in the Standard Model is capable of pinning down a charged lepton into a coherent state that is not a mass eigenstate, in the first place; instead, while the charged lepton from the W boson decay is not initially in a mass eigenstate, neither is it in any "neutrino-centric" eigenstate, nor in any other coherent state. It cannot meaningfully be said that such a featureless charged lepton oscillates or that it does not oscillate, as any "oscillation" transformation would just leave it the same generic state that it was before the oscillation. Therefore, detection of a charged lepton oscillation from W boson decay is infeasible on multiple levels.[19][20]
The idea of neutrino oscillation was first put forward in 1957 by Bruno Pontecorvo, who proposed that neutrino–antineutrino transitions may occur in analogy with neutral kaon mixing.[2] Although such matter–antimatter oscillation had not been observed, this idea formed the conceptual foundation for the quantitative theory of neutrino flavor oscillation, which was first developed by Maki, Nakagawa, and Sakata in 1962[21] and further elaborated by Pontecorvo in 1967.[3] One year later the solar neutrino deficit was first observed,[22] and that was followed by the famous article by Gribov and Pontecorvo published in 1969 titled "Neutrino astronomy and lepton charge".[23]
The concept of neutrino mixing is a natural outcome of gauge theories with massive neutrinos, and its structure can be characterized in general.[24] In its simplest form it is expressed as a unitary transformation relating the flavor and mass eigenbasis and can be written as
where
is a neutrino with definite flavor α = e (electron), μ (muon) or τ (tauon),
is a neutrino with definite mass
the superscript asterisk () represents a complex conjugate; for antineutrinos, the complex conjugate should be removed from the first equation and inserted into the second.
The symbol represents the Pontecorvo–Maki–Nakagawa–Sakata matrix (also called the PMNS matrix, lepton mixing matrix, or sometimes simply the MNS matrix). It is the analogue of the CKM matrix describing the analogous mixing of quarks. If this matrix were the identity matrix, then the flavor eigenstates would be the same as the mass eigenstates. However, experiment shows that it is not.
When the standard three-neutrino theory is considered, the matrix is 3×3. If only two neutrinos are considered, a 2×2 matrix is used. If one or more sterile neutrinos are added (see later), it is 4×4 or larger. In the 3×3 form, it is given by[25]
where cij≡ cos θij, and sij≡ sin θij. The phase factors α1 and α2 are physically meaningful only if neutrinos are Majorana particles—i.e. if the neutrino is identical to its antineutrino (whether or not they are is unknown)—and do not enter into oscillation phenomena regardless. If neutrinoless double beta decay occurs, these factors influence its rate. The phase factor δ is non-zero only if neutrino oscillation violates CP symmetry; this has not yet been observed experimentally. If experiment shows this 3×3 matrix to be not unitary, a sterile neutrino or some other new physics is required.
Propagation and interference
Since are mass eigenstates, their propagation can be described by plane wave solutions of the form
where E is the energy of the wavepacket (particle) to be detected.
This limit applies to all practical (currently observed) neutrinos, since their masses are less than 1 eV and their energies are at least 1 MeV, so the Lorentz factor, γ, is greater than 106 in all cases. Using also t ≈ L, where L is the distance traveled and also dropping the phase factors, the wavefunction becomes
Eigenstates with different masses propagate with different frequencies. The heavier ones oscillate faster compared to the lighter ones. Since the mass eigenstates are combinations of flavor eigenstates, this difference in frequencies causes interference between the corresponding flavor components of each mass eigenstate. Constructive interference causes it to be possible to observe a neutrino created with a given flavor to change its flavor during its propagation. The probability that a neutrino originally of flavor α will later be observed as having flavor β is
This is more conveniently written as
where
The phase that is responsible for oscillation is often written as (with c and restored)
where 1.27 is unitless. In this form, it is convenient to plug in the oscillation parameters since:
The mass differences, Δm2, are known to be on the order of 10−4 eV2 = (10−2 eV)2
Oscillation distances, L, in modern experiments are on the order of kilometers
Neutrino energies, E, in modern experiments are typically on order of MeV or GeV.
If there is no CP-violation (δ is zero), then the second sum is zero. Otherwise, the CP asymmetry can be given as
The above formula is correct for any number of neutrino generations. Writing it explicitly in terms of mixing angles is extremely cumbersome if there are more than two neutrinos that participate in mixing. Fortunately, there are several meaningful cases in which only two neutrinos participate significantly. In this case, it is sufficient to consider the mixing matrix
Then the probability of a neutrino changing its flavor is
Or, using SI units and the convention introduced above
This formula is often appropriate for discussing the transition νμ ↔ ντin atmospheric mixing, since the electron neutrino plays almost no role in this case. It is also appropriate for the solar case of νe ↔ νx , where νxis a mix (superposition) of νμand ντ . These approximations are possible because the mixing angle θ13 is very small and because two of the mass states are very close in mass compared to the third.
Classical analogue of neutrino oscillation
Spring-coupled pendulums
Time evolution of the pendulums
Lower frequency normal mode
Higher frequency normal mode
The basic physics behind neutrino oscillation can be found in any system of coupled harmonic oscillators. A simple example is a system of two pendulums connected by a weak spring (a spring with a small spring constant). The first pendulum is set in motion by the experimenter while the second begins at rest. Over time, the second pendulum begins to swing under the influence of the spring, while the first pendulum's amplitude decreases as it loses energy to the second. Eventually all of the system's energy is transferred to the second pendulum and the first is at rest. The process then reverses. The energy oscillates between the two pendulums repeatedly until it is lost to friction.
The behavior of this system can be understood by looking at its normal modes of oscillation. If the two pendulums are identical then one normal mode consists of both pendulums swinging in the same direction with a constant distance between them, while the other consists of the pendulums swinging in opposite (mirror image) directions. These normal modes have (slightly) different frequencies because the second involves the (weak) spring while the first does not. The initial state of the two-pendulum system is a combination of both normal modes. Over time, these normal modes drift out of phase, and this is seen as a transfer of motion from the first pendulum to the second.
The description of the system in terms of the two pendulums is analogous to the flavor basis of neutrinos. These are the parameters that are most easily produced and detected (in the case of neutrinos, by weak interactions involving the W boson). The description in terms of normal modes is analogous to the mass basis of neutrinos. These modes do not interact with each other when the system is free of outside influence.
When the pendulums are not identical the analysis is slightly more complicated. In the small-angle approximation, the potential energy of a single pendulum system is , where g is the standard gravity, L is the length of the pendulum, m is the mass of the pendulum, and x is the horizontal displacement of the pendulum. As an isolated system the pendulum is a harmonic oscillator with a frequency of . The potential energy of a spring is where k is the spring constant and x is the displacement. With a mass attached it oscillates with a period of . With two pendulums (labeled a and b) of equal mass but possibly unequal lengths and connected by a spring, the total potential energy is
This is a quadratic form in xa and xb, which can also be written as a matrix product:
where λ1 and λ2 are the eigenvalues of the matrix. The variables x1 and x2 describe normal modes which oscillate with frequencies of and . When the two pendulums are identical (La = Lb), θ is 45°.
The angle θ is analogous to the Cabibbo angle (though that angle applies to quarks rather than neutrinos).
When the number of oscillators (particles) is increased to three, the orthogonal matrix can no longer be described by a single angle; instead, three are required (Euler angles). Furthermore, in the quantum case, the matrices may be complex. This requires the introduction of complex phases in addition to the rotation angles, which are associated with CP violation but do not influence the observable effects of neutrino oscillation.
Theory, graphically
Two neutrino probabilities in vacuum
In the approximation where only two neutrinos participate in the oscillation, the probability of oscillation follows a simple pattern:
The blue curve shows the probability of the original neutrino retaining its identity. The red curve shows the probability of conversion to the other neutrino. The maximum probability of conversion is equal to sin22θ. The frequency of the oscillation is controlled by Δm2.
Three neutrino probabilities
If three neutrinos are considered, the probability for each neutrino to appear is somewhat complex. The graphs below show the probabilities for each flavor, with the plots in the left column showing a long range to display the slow "solar" oscillation, and the plots in the right column zoomed in, to display the fast "atmospheric" oscillation. The parameters used to create these graphs (see below) are consistent with current measurements, but since some parameters are still quite uncertain, some aspects of these plots are only qualitatively correct.[26]
The illustrations were created using the following parameter values:[26]
sin2(2θ13) = 0.10 (Determines the size of the small wiggles.)
sin2(2θ23) = 0.97
sin2(2θ12) = 0.861
δ = 0 (If the actual value of this phase is large, the probabilities will be somewhat distorted, and will be different for neutrinos and antineutrinos.)
Normal mass hierarchy: m1 ≤ m2 ≤ m3
Δm2 12 = 0.759×10−4 eV2
Δm2 32 ≈ Δm2 13 = 23.2×10−4 eV2
Observed values of oscillation parameters
sin2(2 θ13) = 0.093±0.008 .[27]PDG combination of Daya Bay, RENO, and Double Chooz results.
sin2(2 θ12) = 0.846±0.021 .[27] This corresponds to θsol (solar), obtained from KamLand, solar, reactor and accelerator data.
sin2(2 θ23″) > 0.92 at 90% confidence level, corresponding to θ23 ≡ θatm = 45±7.1° (atmospheric)[28]
δ, α1, α2, and the sign of Δm2 32 are currently unknown.
Solar neutrino experiments combined with KamLAND have measured the so-called solar parameters Δm2 sol andsin2θsol . Atmospheric neutrino experiments such as Super-Kamiokande together with the K2K and MINOS long baseline accelerator neutrino experiment have determined the so-called atmospheric parameters Δm2 atm and sin2θatm . The last mixing angle, θ13, has been measured by the experiments Daya Bay, Double Chooz and RENO as sin2(2 θ13″) .
For atmospheric neutrinos the relevant difference of masses is about Δm2 = 24.×10−4 eV2and the typical energies are ≈1 GeV; for these values the oscillations become visible for neutrinos traveling several hundred kilometres, which would be those neutrinos that reach the detector traveling through the earth, from below the horizon.
The mixing parameter θ13 is measured using electron anti-neutrinos from nuclear reactors. The rate of anti-neutrino interactions is measured in detectors sited near the reactors to determine the flux prior to any significant oscillations and then it is measured in far detectors (placed kilometres from the reactors). The oscillation is observed as an apparent disappearance of electron anti-neutrinos in the far detectors (i.e. the interaction rate at the far site is lower than predicted from the observed rate at the near site).
From atmospheric and solar neutrino oscillation experiments, it is known that two mixing angles of the MNS matrix are large and the third is smaller. This is in sharp contrast to the CKM matrix in which all three angles are small and hierarchically decreasing. The CP-violating phase of the MNS matrix is as of April 2020 to lie somewhere between −2 and −178 degrees, from the T2K experiment.[29]
If the neutrino mass proves to be of Majorana type (making the neutrino its own antiparticle), it is then possible that the MNS matrix has more than one phase.
Since experiments observing neutrino oscillation measure the squared mass difference and not absolute mass, one might claim that the lightest neutrino mass is exactly zero, without contradicting observations. This is however regarded as unlikely by theorists.
Origins of neutrino mass
The question of how neutrino masses arise has not been answered conclusively. In the Standard Model of particle physics, fermions only have intrinsic mass because of interactions with the Higgs field (see Higgs boson). These interactions require both left- and right-handed versions of the fermion (see chirality). However, only left-handed neutrinos have been observed so far.
Neutrinos may have another source of mass through the Majorana mass term. This type of mass applies for electrically neutral particles since otherwise it would allow particles to turn into anti-particles, which would violate conservation of electric charge.
The smallest modification to the Standard Model, which only has left-handed neutrinos, is to allow these left-handed neutrinos to have Majorana masses. The problem with this is that the neutrino masses are surprisingly smaller than the rest of the known particles (at least 600,000 times smaller than the mass of an electron), which, while it does not invalidate the theory, is widely regarded as unsatisfactory as this construction offers no insight into the origin of the neutrino mass scale.
The next simplest addition would be to add into the Standard Model right-handed neutrinos that interact with the left-handed neutrinos and the Higgs field in an analogous way to the rest of the fermions. These new neutrinos would interact with the other fermions solely in this way and hence would not be directly observable, so are not phenomenologically excluded. The problem of the disparity of the mass scales remains.
The most popular conjectured solution currently is the seesaw mechanism, where right-handed neutrinos with very large Majorana masses are added. If the right-handed neutrinos are very heavy, they induce a very small mass for the left-handed neutrinos, which is proportional to the reciprocal of the heavy mass.
If it is assumed that the neutrinos interact with the Higgs field with approximately the same strengths as the charged fermions do, the heavy mass should be close to the GUT scale. Because the Standard Model has only one fundamental mass scale,[b] all particle masses[c] must arise in relation to this scale.
There are other varieties of seesaw[30] and there is currently great interest in the so-called low-scale seesaw schemes, such as the inverse seesaw mechanism.[31]
The addition of right-handed neutrinos has the effect of adding new mass scales, unrelated to the mass scale of the Standard Model, hence the observation of heavy right-handed neutrinos would reveal physics beyond the Standard Model. Right-handed neutrinos would help to explain the origin of matter through a mechanism known as leptogenesis.
Other sources
There are alternative ways to modify the standard model that are similar to the addition of heavy right-handed neutrinos (e.g., the addition of new scalars or fermions in triplet states) and other modifications that are less similar (e.g., neutrino masses from loop effects and/or from suppressed couplings). One example of the last type of models is provided by certain versions supersymmetric extensions of the standard model of fundamental interactions, where R parity is not a symmetry. There, the exchange of supersymmetric particles such as squarks and sleptons can break the lepton number and lead to neutrino masses. These interactions are normally excluded from theories as they come from a class of interactions that lead to unacceptably rapid proton decay if they are all included. These models have little predictive power and are not able to provide a cold dark matter candidate.
Oscillations in the early universe
During the early universe when particle concentrations and temperatures were high, neutrino oscillations could have behaved differently.[32] Depending on neutrino mixing-angle parameters and masses, a broad spectrum of behavior may arise including vacuum-like neutrino oscillations, smooth evolution, or self-maintained coherence. The physics for this system is non-trivial and involves neutrino oscillations in a dense neutrino gas.
^
More formally, the neutrinos are emitted in an entangled state with the other bodies in the decay or reaction, and the mixed state is properly described by a density matrix. However, for all practical situations, the other particles in the decay may be well localized in time and space (e.g. to within a nuclear distance), leaving their momentum with a large spread. When these partner states are projected out, the neutrino is left in a state that for all intents and purposes behaves as the simple superposition of mass states described here. For more information, seeCohen, Glashow & Ligeti (2009).[17]
^The Standard Model fundamental mass scale can be taken as the scale of SU(2)L × U(1)Y breaking.
^The mass of the electron and the mass of the Z boson are examples of particle masses set by the Standard Model fundamental mass scale.
^De Sabbata, V.; Gasperini, M. (1981). "Neutrino oscillations in the presence of torsion". Il Nuovo Cimento A (1971–1996). 65 (4): 479–500. Bibcode:1981NCimA..65..479S. doi:10.1007/BF02902051.
^ abcdefghMeszéna, Balázs. "Neutrino Oscillations". Wolfram Demonstrations Project. Retrieved 8 October 2015. These images were created with Mathematica. The demonstration allows exploration of the parameters.
^ abcdOlive, K. A.; et al. (Particle Data Group) (2014). "2014 Review of Particle Physics". {{cite journal}}: Cite journal requires |journal= (help)
Ada LovelaceLahirThe Hon. Augusta Ada Byron (1815-12-10)10 Desember 1815London, InggrisMeninggal27 November 1852(1852-11-27) (umur 36)Marylebone, London, InggrisMakamGereja St. Mary Magdalene, Hucknall, NottinghamKebangsaanBritishGelarCountess LovelaceSuami/istriWilliam King-Noel, Earl pertama dari LovelaceAnak Byron King-Noel, Viscount Ockham dan Baron Wentworth ke-12 Anne Blunt, Baroness Wentworth ke-15 Ralph King-Milbanke, Earl ke-2 dari Lovelace Augusta Ada King, Countess Lovelace (1...
В Википедии есть статьи о других людях с фамилией Продан. Даниел Продан Общая информация Полное имя Даниел Клаудиу Продан Прозвище Диди Родился 23 марта 1972(1972-03-23)Сату-Маре, Румыния Умер 16 ноября 2016(2016-11-16) (44 года)Волунтари, Румыния Гражданство Румыния Рост 188 см Позиция защ�...
Hans Brunhart (1991) Hans Brunhart (* 28. März 1945 in Balzers) war vom 26. April 1978 bis zum 26. Mai 1993 während vier Amtsperioden Regierungschef und unter anderem Aussenminister, Bildungsminister sowie Finanzminister Liechtensteins. Er ist verheiratet, hat drei Kinder und ist Mitglied der Vaterländischen Union.[1] Inhaltsverzeichnis 1 Leben 1.1 Ausbildung und Einstieg in die Politik 1.2 Wahlergebnisse 1.3 Meilensteine als Regierungschef 1.4 Nach der Politik 2 Ehrungen (Auswahl)...
هذه المقالة يتيمة إذ تصل إليها مقالات أخرى قليلة جدًا. فضلًا، ساعد بإضافة وصلة إليها في مقالات متعلقة بها. (سبتمبر 2023) هذه مقالة غير مراجعة. ينبغي أن يزال هذا القالب بعد أن يراجعها محرر مغاير للذي أنشأها؛ إذا لزم الأمر فيجب أن توسم المقالة بقوالب الصيانة المناسبة. يمكن أيضاً ت
Montgirod Entidad subnacional MontgirodLocalización de Montgirod en Francia Coordenadas 45°32′07″N 6°35′49″E / 45.535277777778, 6.5969444444444Entidad Comuna de Francia y Comuna delegada • País Francia • Región Auvernia-Ródano-Alpes • Departamento Saboya • Distrito Albertville • Cantón Bourg-Saint-Maurice • Mancomunidad Comunidad de comunas de las Laderas de Aime • Comuna Aime-la-PlagneAlcalde delegado Laure...
Artikel ini sebatang kara, artinya tidak ada artikel lain yang memiliki pranala balik ke halaman ini.Bantulah menambah pranala ke artikel ini dari artikel yang berhubungan atau coba peralatan pencari pranala.Tag ini diberikan pada Desember 2022. Dalam artikel ini, nama keluarganya adalah Lim. Lim Eun-sooLim pada tahun 2019Informasi PribadiMewakili negara South KoreaLahir26 Februari 2003 (umur 20)Seoul, Korea SelatanDaerah asalGyeonggi-do, Korea SelatanTinggi164 m (538 ft 1̺...
2nd episode of the 1st season of Falling Skies The ArmoryFalling Skies episodeTom and his team go in search for Ben.Episode no.Season 1Episode 2Directed byGreg BeemanWritten byGraham YostProduction code102Original air dateJune 19, 2011 (2011-06-19)Guest appearances Bruce Gray as Uncle Scott Dale Dye as Col. Porter Martin Roach as Mike Episode chronology ← PreviousLive and Learn Next →Prisoner of War Falling Skies (season 1)List of episodes The Armory is the s...
Overview of television in Croatia Part of a series on theCulture of Croatia History History of Croatia Kingdom of Croatia Renaissance Illyrian movement People Languages Croatian Traditions Costume Name days in Croatia Mythology Cuisine Easter egg Tamburica Wine Licitar Festivals Sinjska alka Religion Badnjak Our Lady of Sinj Marija Bistrica Our Lady of Međugorje Saint Joseph St. Mark's Church Old Church Slavonic Art Architecture Literature Comics Music and Performing arts Dance Theatre Media...
This article is about the year 1937. For the 2005 EP by Soul-Junk, see 1937 (EP). 1937 January February March April May June July August September October November December Calendar year Millennium: 2nd millennium Centuries: 19th century 20th century 21st century Decades: 1910s 1920s 1930s 1940s 1950s Years: 1934 1935 1936 1937 1938 1939 1940 1937 by topic Subject Animation Archaeology Architecture Art Aviation Awards Comics Film Literature Poetry Meteorology Music Country...
River in Yakutia, Russia For the river of the Alazeya basin, see Arga-Yuryakh (Rassokha). Arga-YuryakhАрга-Юрях / Арҕаа ҮрэхLast stretch of the Arga-Yuryakh Sentinel-2 imageMouth location in Yakutia, RussiaLocationCountryRussiaPhysical characteristicsSource • locationOrulgan RangeVerkhoyansk Range • coordinates69°49′31″N 130°20′48″E / 69.82528°N 130.34667°E / 69.82528; 130.34667 • e...
South Korean actress In this Korean name, the family name is Kim. In the stage name or pen-name, the surname is Chae. Chae Seo-jinBornKim Go-woon (1994-04-30) 30 April 1994 (age 29)Gwangyang, South KoreaEducationSchool of Performing Arts SeoulKorea National University of ArtsOccupationActressYears active2006–presentAgentHuayi Brothers[1]Height169 cm (5 ft 7 in)RelativesKim Ok-vin (sister)Korean nameHangul김고운Revised RomanizationKim GounMcCune–Reischau...
Maltese football club For football clubs with a similar name, see Saint George (disambiguation). Football clubSt. George'sFull nameSt. George's Football ClubNickname(s)The PioneersFounded1890; 133 years ago (1890)GroundCentenary Stadium, MaltaCapacity2,000ManagerMaurice PaceLeagueNational Amateur League2021–22Maltese Challenge League, Group A, 11th (relegated) )[1]WebsiteClub website Home colours Away colours The oldest known photograph of the club, taken in 1894 a...
Annual music awards show NME AwardsCurrent: NME Awards 2023Logo for the 2016 NME AwardsCountryUnited KingdomFirst awarded24 April 1953; 70 years ago (1953-04-24)Websitehttp://www.nme.com/awardsTelevision/radio coverageNetworkITV The NME Awards is an annual music awards show in the United Kingdom, founded by the music magazine NME (New Musical Express). The first awards show was held in 1953 as the NME Poll Winners Concerts, shortly after the founding of the magazine. Though ...
For the 2023 animated film, see Mavka: The Forest Song. 1911/1918 play by Lesya Ukrainka This article has multiple issues. Please help improve it or discuss these issues on the talk page. (Learn how and when to remove these template messages) This article needs additional citations for verification. Please help improve this article by adding citations to reliable sources. Unsourced material may be challenged and removed.Find sources: The Forest Song – news · newspapers&...
American politician Beau BoulterMember of the U.S. House of Representativesfrom Texas's 13th districtIn officeJanuary 3, 1985 – January 3, 1989Preceded byJack HightowerSucceeded byBill Sarpalius Personal detailsBornEldon Beau Boulter (1942-02-23) February 23, 1942 (age 81)El Paso, Texas, U.S.Political partyRepublicanAlma materUniversity of Texas at AustinBaylor Law School Eldon Beau Boulter (born February 23, 1942)[1] is an American politician.[2]...
Japanese judoka The neutrality of this article is disputed. Relevant discussion may be found on the talk page. Please do not remove this message until conditions to do so are met. (January 2021) (Learn how and when to remove this template message) Hitoshi SaitoSaito at the 1988 Summer OlympicsPersonal informationBornJanuary 2, 1961Aomori, JapanDiedJanuary 20, 2015 (aged 54)Osaka, JapanOccupationJudokaHeight1.80 m (5 ft 11 in)Weight143 kg (315 lb)SportCountryJapanSport...
1983 book by Janet and Isaac Asimov First edition (publ. Walker Books)Cover by Anthony Accardo[1] Norby, the Mixed-Up Robot (1983, Walker & Company) is the first book in the Norby series by Janet Asimov and Isaac Asimov. In it, Jefferson Wells and Norby stop Ing from taking over the Solar System with the help of Jeff's brother Fargo Wells, police officer Albany Jones, and Admiral Boris Yobo. According to Isaac Asimov, although Janet Asimov did 90% of the work, his name was wanted ...
Woman's foundation garment combining bra and girdle For the part of a standard diving dress, see Standard diving dress § Corselet. Not to be confused with corslet. The inside of a corselette In women's clothing, a corselet or corselette is a type of foundation garment, sharing elements of both bras and girdles. It extends from straps over the shoulders down the torso, and stops around the top of the legs. It may incorporate lace in front or in back. As an undergarment, a corselet can be...
Athletics at the Olympics Men's standing triple jumpat the Games of the II OlympiadRay EwryVenueBois de BoulogneDateJuly 16Competitors10 from 4 nationsWinning distance10.58 ORMedalists Ray Ewry United States Irving Baxter United States Robert Garrett United States1904 → Athletics at the1900 Summer OlympicsTrack events60 mmen100 mmen200 mmen400 mmen800 mmen1500 mmen110 m hurdlesmen200 m hurdlesmen400 m hurdlesmen2500 m steeplechasemen4000 m steeplechasemen50...
Kazimieras Steponas Šaulys Kazimieras Steponas Šaulys (pengucapan Lituania: [kɐzʲɪˈmʲierɐs ˈstʲæːpɒnɐs ʃauˈlʲîːs] ( simak); 1872 – 9 Mei 1964) adalah seorang imam Katolik Roma, teolog, dan salah satu dari dua puluh penandatangan Undang-Undang Kemerdekaan Lituania. Ia lulus dari Seminar Teologi di Kaunas pada 1895 dan meraih gelar master dari Seminari Teologi Katolik Roma di Sankt-Peterburg pada 1899. Referensi Šaulys, Kazimieras. Encyclopedia Lituanica V: 79-80...