Proton Luminosity Research Articles

Determining the inelastic proton–proton cross section at the large hadron collider using minimum bias events

In this paper a new method is described for determining the non-diffractive part of the inelastic proton–proton cross section, at the LHC centre of mass energy of 14 TeV. The method is based on counting the number of inelastic proton–proton interactions in the collision regions. According to a preliminary investigation, this measurement will be best suited for the initial low luminosity phase of the LHC. Knowledge of the proton–proton luminosity is likely to dominate the measurement uncertainty.

Luminosity measurement in the interaction regions of the LHC using proton–proton collision multiplicities

Described in this article is a new method for determining the absolute proton luminosity at the Large Hadron Collider. The method is based on counting the number of inelastic proton–proton interactions in a bunch crossing. We show that this should be possible using the inner detector systems of the ATLAS and CMS experiments. Dedicated luminosity instrumentation is not required. The method is best suited for the initial low luminosity phase of the LHC, but its application at high luminosity is also considered.

RHIC performance and future plans

The relativistic heavy ion collider (RHIC) at Brookhaven National Laboratory, consisting of two 3.8km long superconducting rings, was commissioned in 1999. Since then the machine collided fully stripped gold ions at five different energies, up to 100GeV/n, deuterons with gold ions at 100GeV/n and protons at 100GeV with a beam polarizations of up 45%. Over four operating periods the heavy ion luminosity has increased by two orders of magnitude, and now exceeds the design value by a factor of two. Another factor of two is targeted for the next four years, as well as a more than 10-fold increase in the proton luminosity and a 2-fold increase in the polarization. Possible further upgrades include an electron beam ion source (EBIS), stochastic and electron cooling and an electron ring to form an electron–ion collider (eRHIC).

Physics potential of the Fermilab NuMI beamline

We explore the physics potential of the NuMI beamline with a detector located 10 km off axis at a distant site (810 km). We study the sensitivity to ${sin}^{2}2{\ensuremath{\theta}}_{13}$ and to the $CP$-violating parameter $\mathrm{sin}\ensuremath{\delta}$ as well as the determination of the neutrino mass hierarchy by exploiting the ${\ensuremath{\nu}}_{\ensuremath{\mu}}\ensuremath{\rightarrow}{\ensuremath{\nu}}_{e}$ and ${\overline{\ensuremath{\nu}}}_{\ensuremath{\mu}}\ensuremath{\rightarrow}{\overline{\ensuremath{\nu}}}_{e}$ appearance channels. The results are illustrated for three different experimental setups to quantify the benefits of increased detector sizes, proton luminosities, and ${\ensuremath{\nu}}_{e}$ detection efficiencies.

Problems of ultra-high-energy particle acceleration in Cygnus X-3 - A critical reappraisal

view Abstract Citations (19) References (39) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Problems of Ultra--High-Energy Particle Acceleration in Cygnus X-3: A Critical Reappraisal Mitra, Abhas Abstract All the major viable acceleration mechanisms suggested so far in order to explain the energy of the gamma-rays observed from Cygnus X-3 are critically reviewed. It is argued that Cyg X-3 must be an accretion-fed strong X-ray binary with negligible orbital eccentricity and cannot contain a young active pulsar. It is shown that, for reasonable assumptions, the accretion disk unipolar inductor model can be ruled out as the gamma-ray source in Cyg X-3. It is confirmed that, within the framework of standard magnetospheric theories, there is little scope for extremely efficient diffusive acceleration at the accretion shock. It is concluded that the basic 'beam-dumping' model cannot be applicable to Cyg X-3, and that the proton luminosity requirements of the source can be met if the TeV-PeV gamma-ray flux is generated by photomeson reaction on its strong X-ray field. Publication: The Astrophysical Journal Pub Date: March 1991 DOI: 10.1086/169821 Bibcode: 1991ApJ...370..345M Keywords: Energetic Particles; Gamma Ray Astronomy; Particle Acceleration; Pulsars; X Ray Binaries; Accretion Disks; Computational Astrophysics; Shock Waves; Stellar Evolution; Stellar Luminosity; Stellar Mass Accretion; Astrophysics; GAMMA RAYS: GENERAL; PARTICLE ACCELERATION; PULSARS; RADIATION MECHANISMS; STARS: ACCRETION; STARS: INDIVIDUAL CONSTELLATION NAME: CYGNUS X-3; X-RAYS: BINARIES full text sources ADS | data products SIMBAD (5)

Search for 100 TeV gamma-rays from SN 1987 A

We present the results of a search for very high energy γ-rays (E γ≈100 TeV) from SN 1987A between August 1987 and May 1988. No counting rate excess from the source is observed. The larger enhancement is seen in January 1988, but is statistically not significant (1.4 s.d.). The derived upper limits to the γ-ray and proton luminosities of the SN areL γ≤1.9·1040 erg/s andL p≤1.2·1042 erg/s.

Burst of TeV gamma rays from SN 1987A: Cosmic storage rings?

The JANZOS Collaboration has reported a 2-day burst of TeV \ensuremath{\gamma} rays from SN 1987 A 11 months after the explosion. At this supernova epoch TeV \ensuremath{\gamma} rays can only be produced by inelastic proton interactions and secondary ${\ensuremath{\pi}}^{0}$ decay. The proton luminosity during the burst has to be 2\ifmmode\times\else\texttimes\fi{}${10}^{39}$ ergs/s, in contradiction with the most recent estimates of the total power of an internal energy source. We suggest a burst model where the TeV \ensuremath{\gamma}-ray burst is produced by a previously accumulated proton beam, which is in agreement with the observed energetics of SN 1987A in all observation bands.

Search for Ultra-High-Energy Gamma-Rays from SN1987A

AbstractWe report here a search of data recorded by the Buckland Park air shower array from the first year after the supernova and set an upper limit to the proton luminosity of SN1987A of 7.7 × 1040 ergs s−1.

On the possibility of observations of high energy neutrino and gamma-ray fluxes from SN1987A

We estimate the production of high energy neutrino and gamma-ray signals through interactions of protons and subsequent decay of secondaries in the shell of SN1987a. We also discuss the absorption of the gamma-ray signals, the detection limits and the existing and proposed experiments in the Southern hemisphere, TeV and PeV gamma-ray signals will be detectable if the total proton luminosity of the supernova is greater than 10 39 erg/s and the differential spectral index γ of the accelerated protons is not steeper than 2.4. The detection of neutrino induced muons from the supernova will only be possible if the total proton luminosity exceeds 10 42 erg/s.