Search results for "W-MASS"

showing 3 items of 13 documents

Measurement of trilinear gauge boson couplings WWV, (V Z,gamma) in e(+)e(-) collisions at 189 GeV

2001

Measurements of the trilinear gauge boson couplings WWgamma and WWZ are presented using the data taken by DELPHI in 1998 at a centre-of-mass energy of 189 GeV and combined with DELPHI data at 183 GeV. Values are determined for Delta(g_1^Z) and Delta(kappa_gamma), the differences of the WWZ charge coupling and of the WWgamma dipole coupling from their Standard Model values, and for lambda_gamma, the WWgamma quadrupole coupling. A measurement of the magnetic dipole and electric quadrupole moment of the W is extracted from the results for Delta(kappa_gamma) and lambda_gamma. The study uses data from the final states jjlv, jjjj, lX, jjX and gammaX, where j represents a quark jet, l an identifie…

QuarkNuclear and High Energy PhysicsParticle physicsENERGIESAstrophysics::High Energy Astrophysical Phenomenastandard modelLEP-IIFOS: Physical sciencesLambda7. Clean energy01 natural sciencesPartícules (Física nuclear)High Energy Physics - ExperimentStandard ModelEVENTSHigh Energy Physics - Experiment (hep-ex)BHABHA SCATTERINGMONTE-CARLO0103 physical sciencesOPTIMAL OBSERVABLES[PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex]W-MASSgauge couplings010306 general physicsDETECTORQCDELPHIPhysicsGauge boson010308 nuclear & particles physicsHigh Energy Physics::PhenomenologyCharge (physics)LARGE ELECTRON POSITRON COLLIDERFIS/01 - FISICA SPERIMENTALECol·lisions (Física nuclear)QuadrupolePARTICLE PHYSICS; LARGE ELECTRON POSITRON COLLIDER; DELPHIOPTIMAL OBSERVABLES; BHABHA SCATTERING; MONTE-CARLO; W-MASS; LEP-II; EVENTS; DETECTOR; DELPHI; E+E-->W+W; ENERGIESelectron-positron collisionPARTICLE PHYSICSFísica nuclearHigh Energy Physics::ExperimentE+E-->W+WMagnetic dipoleLepton
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Mapping accretion and its variability in the young open cluster NGC 2264: A study based on u-band photometry

2014

We aim at characterizing the accretion properties of several hundred members of the star-forming cluster NGC 2264 (3 Myr). We performed a deep u,g,r,i mapping and a simultaneous u+r monitoring of the region with CFHT/MegaCam in order to directly probe the accretion process from UV excess measurements. Photometric properties and stellar parameters are determined homogeneously for about 750 monitored young objects, spanning the mass range 0.1-2 Mo. About 40% are classical (accreting) T Tauri stars, based on various diagnostics (H_alpha, UV and IR excesses). The remaining non-accreting members define the (photospheric+chromospheric) reference UV emission level over which flux excess is detecte…

Stellar massAstrophysics::High Energy Astrophysical PhenomenaStars: formationPopulationFOS: Physical sciencesAstrophysicsAstrophysics::Cosmology and Extragalactic AstrophysicsPhotometry (optics)Accretion rateAccretion accretion diskStars: low-maAstrophysics::Solar and Stellar AstrophysicseducationAstrophysics::Galaxy AstrophysicsSolar and Stellar Astrophysics (astro-ph.SR)Physicseducation.field_of_studyDetection thresholdAstronomy and AstrophysicsAstronomy and AstrophysicUltraviolet: starAccretion (astrophysics)T Tauri starAstrophysics - Solar and Stellar Astrophysicsindividual: NGC 2264; Stars: formation; Stars: low-mass; Stars: pre-main sequence; Ultraviolet: stars; Astronomy and Astrophysics; Space and Planetary Science [Accretion accretion disks; Open clusters and associations]Space and Planetary ScienceOpen clusters and associations: individual: NGC 2264Stars: pre-main sequenceAstrophysics::Earth and Planetary AstrophysicsOpen cluster
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PLANETS AROUND LOW-MASS STARS AND STELLAR ACTIVITY EFFECTS

In the last years the field of exoplanet research has focused its interest in M dwarfs. These stars have became the favourite targets in radial velocity surveys, specially when looking for small planets in the habitable zones of their parent stars. Not only for being the M dwarfs the most common objects in our Galaxy also because the Doppler signals due to small planets orbiting around them are larger and more easily detectable than those around FGK stars. However, stellar magnetic activity and rotation affect the measured radial velocities as surface inhomogeneities rotating with the stellar surface can cause periodic changes in the spectral line centroid. Disentangle these stellar activit…

activity - Stars: low-mass - Techniques: radial velocities - planetary systems [Stars]Stars: activity - Stars: low-mass - Techniques: radial velocities - planetary systems
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