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Raj Gandhi

Publications and source records attributed to Raj Gandhi.

At least 55 records · Page 3Linked to original sources

Physics with a very long neutrino factory baseline

We discuss the neutrino oscillation physics of a very long neutrino factory baseline over a broad range of lengths (between 6000 km and 9000 km), centered on the ``magic baseline'' ($\sim$ 7500 km) where correlations with the leptonic CP phase are suppressed by matter effects. Since the magic baseline depends only on the density, we study the impact of matter density profile effects and density uncertainties over this range, and the impact of detector locations off the optimal baseline. We find that the optimal constant density describing the physics over this entire baseline range is about 5% higher than the average matter density. This implies that the magic baseline is significantly shorter than previously inferred. However, while a single detector optimization requires fine-tuning of the (very long) baseline length, its combination with a near detector at a shorter baseline is much less sensitive to the far detector location and to uncertainties in the matter density. In addition, we point out different applications of this baseline which go beyond its excellent correlation and degeneracy resolution potential. We demonstrate that such a long baseline assists in the improvement of the $θ_{13}$ precision and in the resolution of the octant degeneracy. Moreover, we show that the neutrino data from such a baseline could be used to extract the matter density along the profile up to 0.24% at $1 σ$ for large $\sin^2 2 θ_{13}$, providing a useful discriminator between different geophysical models.

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Probing Very High Energy Prompt Muon and Neutrino fluxes and the cosmic ray knee via Underground Muons

We calculate event rate and demonstrate the observational feasibility of very high energy muons (1-1000 TeV) in a large mass underground detector operating as a pair-meter. This energy range corresponds to surface muon energies of $\sim$(5 TeV - 5000 TeV) and primary cosmic ray energies of $\sim$ (50 TeV - 5 $\times 10^4$ TeV). Such measurements would significantly assist in an improved understanding of the prompt contribution to $ν_e, ν_μ$ and $μ$ fluxes in present and future ultra-high energy neutrino detectors. In addition, they would shed light on the origin of the observed 'knee' in the cosmic ray spectrum.

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Earth Matter Effects at Very Long Baselines and the Neutrino Mass Hierarchy

We study matter effects which arise in the muon neutrino oscillation and survival probabilities relevant to atmospheric neutrino and very long baseline beam experiments. The inter-relations between the three probabilities P_{μe}, P_{μτ} and P_{μμ} are examined. It is shown that large and observable sensitivity to the neutrino mass hierarchy can be present in P_{μμ} and P_{μτ}. We emphasize that at baselines of > 7000 Km, matter effects in P_{μτ} can be large under certain conditions. The muon survival rates in experiments with very long baselines thus depend on matter effects in both P_{μτ} and P_{μe}. We indicate where these effects are sensitive to θ_{13}, and identify ranges of E and L where the event rates increase with decreasing θ_{13}, providing a handle to probe small θ_{13}. The effect of parameter degeneracies in the three probabilities at these baselines and energies is studied in detail. Realistic event rate calculations are performed for a charge discriminating 100 kT iron calorimeter which demonstrate the possibility of realising the goal of determining the neutrino mass hierarchy using atmospheric neutrinos. It is shown that a careful selection of energy and baseline ranges is necessary in order to obtain a statistically significant signal, and that the effects are largest in bins where matter effects in both P_{μe} and P_{μτ} combine constructively. Under these conditions, upto a 4σsignal for matter effects is possible (for Δ_{31}>0) within a timescale appreciably shorter than the one anticipated for neutrino factories.

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Probing the Neutrino Mass Hierarchy via Atmospheric $ν_μ+ \bar ν_μ$ Survival Rates in Megaton Water Cerenkov Detectors

The neutrino mass hierarchy, presently unknown, is a powerful discriminator among various classes of unification theories. We show that the $ν_μ + \barν_μ$ survival rate in atmospheric events can provide a novel method of determining the hierarchy in megaton water Cerenkov detectors. For pathlength and energy ranges relevant to atmospheric neutrinos,this rate obtains significant matter sensitive variations not only from resonant matter effects in $P_{μe}$ but also from those in $P_{μτ}$. We calculate the expected muon event rates in the case of matter oscillations with both natural and inverted hierarchy.We identify the energy and pathlength ranges for which resonant matter effects can lead to observable differences between the above two cases. We also estimate the exposure time required to observe this difference and determine the sign of $Δ_{31}$ in a statistically significant manner.

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Large Matter Effects in ${ν_μ\to ν_τ}$ Oscillations

We show that matter effects change the ${\rm {ν_μ\to ν_τ}}$ oscillation probability by as much as 70% for certain ranges of energies and pathlengths. Consequently, the ${\rm {ν_μ\to ν_μ}}$ survival probability also undergoes large changes. A proper understanding of $ν_μ$ survival rates must consider matter effects in $P_{μτ}$ as well as $P_{μe}$. We comment on a) how these matter effects may be observed and the sign of $Δ_{31}$ determined in atmospheric neutrino measurements and at neutrino factories and b) how they lead to heightened sensitivity for small $θ_{13}$.

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Atmospheric Neutrinos as a Probe of CPT Violation

We show that atmospheric neutrinos can provide a sensitive and robust probe of CPT violation (CPTV). We perform realistic event-rate calculations and study the variations of the ratio of total muon to antimuon survival rates with $L/E$ and $L$ ($L$ $\equiv$ baseline length, $E$ $\equiv$ neutrino energy) in a detector capable of identifying the muon charge. We demonstrate that measurements of these ratios when coupled with the significant $L$ and $E$ range which characterizes the atmospheric neutrino spectrum provides a method of both detecting the presence of such violations and putting bounds on them which compare very favourably with those possible from a future neutrino factory.

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Testing the solar LMA region with KamLAND data

We investigate the potential of 3 kiloTon-years(kTy) of KamLAND data to further constrain the $Δm^2$ and $\tan^2θ$ values compared to those presently allowed by existing KamLAND and global solar data. We study the extent, dependence and characteristics of this sensitivity in and around the two parts of the LMA region that are currently allowed. Our analysis with 3 kTy simulated spectra shows that KamLAND spectrum data by itself can constrain $Δm^2$ with high precision. Combining the spectrum with global solar data further tightens the constraints on allowed values of $\tan^2θ$ and $Δm^2$. We also study the effects of future neutral current data with a total error of 7% from the Sudbury Neutrino Observatory. We find that these future measurements offer the potential of considerable precision in determining the oscillation parameters (specially the mass parameter).

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The Solar Neutrino Problem after the first results from Kamland

The first results from the KamLAND experiment have provided confirmational evidence for the Large Mixing Angle (LMA) MSW solution to the solar neutrino problem. We do a global analysis of solar and the recently announced KamLAND data (both rate and spectrum) and investigate its effect on the allowed region in the $Δm^2-\tan^2θ$ plane. The best-fit from a combined analysis which uses the KamLAND rate plus global solar data comes at $Δm^2 = 6.06 \times 10^{-5}$ eV $^2$ and $\tan^2θ=0.42$, very close to the global solar best-fit, leaving a large allowed region within the global solar LMA contour. The inclusion of the KamLAND spectral data in the global fit gives a best-fit $Δm^2 = 7.15 \times 10^{-5}$ eV $^2$ and $\tan^2θ=0.42$ and constrains the allowed areas within LMA, leaving essentially two allowed zones. Maximal mixing though allowed by the KamLAND data alone is disfavored by the global solar data and remains disallowed at about $3σ$. The LOW solution is now ruled out at about 5$σ$ w.r.t. the LMA solution.

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Signals of R-parity Violating Supersymmetry at a Muon Storage Ring

Neutrino oscillation signals at muon storage rings (MSR) can be mimicked by Supersymmetric (SUSY) interactions in an R-parity violating scenario. We have investigated the $τ$-appearance signals for both long-baseline and near-site experiments, and concluded that the latter is of great use in distinguishing between oscillation and SUSY effects. On the other hand, SUSY can cause a manifold increase in the event rate for wrong-sign muons at a long-baseline setting, thereby providing us with signatures of new physics.

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Signals of R-parity violating supersymmetry in neutrino scattering at muon storage rings

Neutrino oscillation signals at muon storage rings can be faked by supersymmetric (SUSY) interactions in an R-parity violating scenario. We investigate the $τ$-appearance signals for both long-baseline and near-site experiments, and conclude that the latter is of great use in distinguishing between oscillation and SUSY effects. On the other hand, SUSY can cause a manifold increase in the event rate for wrong-sign muons at a long-baseline setting, thereby providing us with signatures of new physics.

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Ultra-High Energy Neutrinos: A Review of Theoretical and Phenomenological Issues

We review the phenomenology of ultra-high energy (UHE) neutrino detection. The motivations for looking for such neutrinos stemming from observational evidence and the potential for new physics discoveries are enumerated, and their expected sources and fluxes are given. Cross-sections with nucleons all the way upto neutrino energies of 10^20 eV, and the attenuation of the fluxes in the earth are discussed. Finally, sample event-rates for existing and future Water/Ice Cerenkov detectors are provided.

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Tau-neutrino Appearance Searches using Neutrino Beams from Muon Storage Rings

We study the possibilities offered by muon storage rings for tau-neutrino appearance experiments due to nu_mu to nu_tau and nu_e to nu_tau oscillations. Tau event rates for such experiments are first discussed with a view to examining their variation prior to the inclusion of experimental cuts, in order to better understand how baselines, beam energies, forward peaking of decay neutrinos with increasing energies and average fluxes intercepted by detectors of various sizes can affect their optimization. Subsequently, event rates implementing cuts are computed for hadronic and wrong-sign lepton decay modes and used to plot 90% C.L. contours for the parameters that can be explored in such experiments. The expected scaling of the contours with energy and baseline is discussed. The results show that even for modest muon beam energies, convincing coverage of the Super Kamiokande parameters is possible. In addition, very significant enlargement of present-day bounds on the mass and mixing parameters of all types of neutrino oscillations is guaranteed by such searches.

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Neutrino Interactions at Ultrahigh Energies

We report new calculations of the cross sections for deeply inelastic neutrino-nucleon scattering at neutrino energies between $10^{9}\ev$ and $10^{21}\ev$. We compare with results in the literature and assess the reliability of our predictions. For completeness, we briefly review the cross sections for neutrino interactions with atomic electrons, emphasizing the role of the $W$-boson resonance in $\barν_{e}e$ interactions for neutrino energies in the neighborhood of $6.3\pev$. Adopting model predictions for extraterrestrial neutrino fluxes from active galactic nuclei, gamma-ray bursters, and the collapse of topological defects, we estimate event rates in large-volume water Čerenkov detectors and large-area ground arrays.

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Detecting Neutrinos from AGNs and Topological Defects with Neutrino Telescopes

We evaluate neutrino-nucleon cross section for energies up to $10^{21} eV$ in light of new information on the small-$x$ behavior of parton distributions. We give predictions for large underground neutrino telescope event rates for ultrahigh-energy neutrinos from Active Galactic Nuclei and from the decay of topological defects formed in the early Universe.

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Ultrahigh-Energy Neutrino Interactions and Neutrino Telescope Event Rates

We present results for neutrino-nucleon cross sections for energies up to 10$^21$eV, of relevance to the detection of ultrahigh energy galactic and extragalactic neutrinos. At the highest energies, our results are about 2.4 times larger than previous estimates. Using these new cross sections, we predict neutrino telescope event rates for the upward moving muons initiated by the neutrino interactions in the Earth and for contained-vertex events in the PeV range due to neutrino-electron interactions. We show that future neutrino detectors, such as AMANDA, BAIKAL, DUMAND and NESTOR have a very good chance of detecting neutrinos which originate in the Active Galactic Nuclei.

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New Predictions for Neutrino Telescope Event Rates

Recent measurements of the small-$x$ deep-inelastic regime at HERA translate to new expectations for the neutrino-nucleon cross section at ultrahigh energies. We present event rates for large underground neutrino telescopes based on the new cross section for a variety of models of neutrino production in Active Galactic Nuclei, and we compare these rates with earlier cross section calculations.

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Ultrahigh-Energy Neutrino Interactions

Cross sections for the interactions of ultrahigh-energy neutrinos with nucleons are evaluated in light of new information about nucleon structure functions. For $10^{20}$--eV neutrinos, the cross section is about 2.4 times previous estimates. We also review the cross sections for neutrino interactions with atomic electrons. Some consequences for interaction rates in the Earth and for event rates from generic astrophysical sources in large-scale detectors are noted.

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Small-x Parton Densities from HERA and the Ultra-High Energy Neutrino-Nucleon Cross Sections

In light of recent measurements of the nucleon structure function in the small-$x$ deep-inelastic regime at HERA and the consequently improved theoretical understanding of the quark distributions in this range of parton fractional momentum, we present new results for the neutrino-nucleon cross section at ultra high energies, up to $ E_ν \sim 10^{21}$ eV. The results are relevant to deep underground muon detectors looking for such neutrinos. For $\simeq 10^{20}$ eV neutrinos, our cross sections are about a factor of $4$ to $10$ times larger than the previously reported results by Reno, Quigg and Walker. We discuss implications of this new neutrino-nucleon cross section for a variety of current and future neutrino detectors.

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