Search results for "Jets"

Expositio missae : le commentaire du Canon de la Messe dans la tradition monastique et scolastique

2003

Place: Auxerre Publisher: Centre d'études médiévales

Théologie eucharistique et valorisation de l'autel à l'Âge roman

2005

First Observation of Top Quark Production in the Forward Region

2015

Top quark production in the forward region in proton-proton collisions is observed for the first time. The W + b final state with W → μν is reconstructed using muons with a transverse momentum, p[subscript T], larger than 25 GeV in the pseudorapidity range 2.0 20  GeV. The results are based on data corresponding to integrated luminosities of 1.0 and 2.0  fb[superscript -1] collected at center-of-mass energies of 7 and 8 TeV by LHCb. The inclusive top quark production cross sections in the fiducial region are σ(top)[7  TeV] = 239 ± 53(stat) ± 33(syst) ± 24(theory)  fb, σ(top)[8  TeV] = 289 ± 43(stat) ± 40(syst) ± 29(theory)  fb.These results, along with the observed differential yields and c…

"Table 8" of "Energy dependence of event shapes and of alpha(s) at LEP-2."

1999

Moments of the Wide Jet Broadening (BMAX) distributions at cm energies 133, 161, 172 and 183 GeV.

"Table 12" of "Energy dependence of event shapes and of alpha(s) at LEP-2."

1999

Moments of the C-parameter (C-PARAM) distributionss at cm energies 133, 161, 172 and 183 GeV.

"Table 2" of "Energy dependence of event shapes and of alpha(s) at LEP-2."

1999

Moments of the Thrust Major distributions at cm energies 133, 161, 172 and 183 GeV.

"Table 6" of "Energy dependence of event shapes and of alpha(s) at LEP-2."

1999

Moments of the Light Jet Mass (ML**2/EVIS**2) distributions at cm energies 133, 161, 172 and 183 GeV.

Simultaneous radio and X-ray observations of the low-mass X-ray binary GX 13+1

2004

We present the results of two simultaneous X-ray/radio observations of the low-mass X-ray binary GX 13+1, performed in July/August 1999 with the Rossi X-ray Timing Explorer and the Very Large Array. In X-rays the source was observed in two distinct spectral states; a soft state, which had a corresponding 6 cm flux density of ~0.25 mJy, and a hard state, which was much brighter at 1.3-7.2 mJy. For the radio bright observation we measured a delay between changes in the X-ray spectral hardness and the radio brightness of ~40 minutes, similar to what has been found in the micro-quasar GRS 1915+105. We compare our results with those of GRS 1915+105 and the atoll/Z-type neutron star X-ray binarie…

3D simulations of wind-jet interaction in massive X-ray binaries

2010

High-mass microquasars may produce jets that will strongly interact with surrounding stellar winds on binary system spatial scales. We study the dynamics of the collision between a mildly relativistic hydrodynamical jet of supersonic nature and the wind of an OB star. We performed numerical 3D simulations of jets that cross the stellar wind with the code Ratpenat. The jet head generates a strong shock in the wind, and strong recollimation shocks occur due to the initial overpressure of the jet with its environment. These shocks can accelerate particles up to TeV energies and produce gamma-rays. The recollimation shock also strengthens jet asymmetric Kelvin-Helmholtz instabilities produced i…

Tracking the evolution of the accretion flow in MAXI J1820+070 during its hard state with the JED-SAD model

2021

X-ray binaries in outburst typically show two canonical X-ray spectral states, i.e. hard and soft states, in which the physical properties of the accretion flow and of the jet are known to change. Recently, the JED-SAD paradigm has been proposed for black hole X-ray binaries, aimed to address the accretion-ejection interplay in these systems. According to this model, the accretion flow is composed by an outer standard Shakura-Sunyaev disk (SAD) and an inner hot Jet Emitting Disk (JED). The JED produces both the hard X-ray emission, effectively playing the role of the hot corona, and the radio jets. In this paper, we use the JED-SAD model to describe the evolution of the accretion flow in th…