arXiv subjects

Nickolas Solomey

Publications and source records attributed to Nickolas Solomey.

10 recordsLinked to original sources

arXiv2026

SNAPPY CubeSat Control Script Generation and Data File Processing

This is a document discussing the creation and usage of a server system dedicated to retrieving, processing, and storing data generated from the Solar Neutrino and Astro-Particle PhYsics (SNAPPY) CubeSat by the nuSOL (Neutrino Solar Orbiting Laboratory) Project. On a traditional desktop computer with CERN's ROOT and PostgreSQL software installed, and with a file system on two mirrored drives, it is possible to automatically process and organize incoming data, along with keeping a database to record each incoming file along with a command record. In addition to this, an application was created to provide a Graphical User Interface to assist with creating commands to communicate with the CubeSat. With that said, there are still plenty of plans to improve the software, mainly providing an automatic emailing system to notify team members when they are not around the server.

astro-ph.IM↗

arXiv2025

Segment Geometry Optimization and Prototype Studies of a Multi-Coincidence GAGG Solar Neutrino Detector

A GAGG detector capable of dissecting a multi-coincidence solar neutrino interaction on ${}^{71}$Ga is under development for potential space-based applications. We identify three distinct detection signatures when ${}^{71}$Ge$^*$ is produced, two of which are significantly delayed in time and could be detected within a single large GAGG volume. Further optimizations can be made by optically isolating smaller segments of GAGG to maximize the probability of a spatial separation between the prompt/delayed signals. We construct and test prototype GAGG detectors capable of sub 7% energy resolution @ ${}^{137}$Cs and reliable detection of spatially-separated ${}^{57}$Co double-pulse decays.

hep-ex↗

arXiv2024

Simulation of Solar Wind Charged Particle Energy Deposited and Particle Identification by $\Delta$E-E Discrimination in the SNAPPY Cubesat Detector

The Solar Neutrino and Astro-Particle PhYsics (SNAPPY) Cubesat is expected to launch in 2025 and it will carry into a polar orbit a prototype test detector for solar neutrino background studies while over the Earth's poles for the neutrino Solar Orbiting Laboratory future project ($\nu$SOL). During this flight it is possible to do other science measurements. One of these is an improved study of the solar wind particles through better particle identification and energy measurements. This study aimed to understand how well could the solar wind particles be identified using the planned detector but instead of using the veto array as an anti-coincidence it would be used as a $\Delta$E energy sampling of a phoswich particle ID system.

astro-ph.SR↗

arXiv2024

New methods of neutrino and anti-neutrino detection from 0.115 to 105 MeV

We have developed a neutrino detector with threshold energies from ~0.115 to 105 MeV in a clean detection mode almost completely void of accidental backgrounds. It was initially developed for the NASA $\nu$SOL project to put a solar neutrino detector very close to the Sun with 1,000 to 10,000 times higher solar neutrino flux than on Earth. Similar interactions have been found for anti-neutrinos, which were initially intended for Beta decay neutrinos from reactors, geological sources, or for nuclear security applications. These techniques work at the 1 to 100 MeV region for neutrinos from the ORNL Spallation Neutron Source or low energy accelerator neutrino and anti-neutrino production targets less than $\sim$100 MeV. The identification process is clean, with a double pulse detection signature within a time window between the first interaction producing the conversion electron or positron and the secondary gamma emission 100 ns to ~1 $\mu$s, which removes most accidental backgrounds. These new modes for neutrino and anti-neutrino detection of low energy neutrinos and anti-neutrinos could allow improvements to neutrino interaction measurements from an accelerator beam on a target.

physics.ins-det↗

arXiv2024

Gamma Ray Detection Efficiency of GAGG Crystal Scintillator Using Three Tagged Gamma Ray Techniques

A CubeSat with a prototype scintillating detector with a sensitive volume of GAGG crystal is being developed with a possible launch date of 2025. Its purpose is to characterize the background signals that mimic the neutrino interaction that the nuSOL (Neutrino Solar Orbiting Laboratory) team is looking for. An important part of the characterization of the backgrounds and the expected real signal is understanding the gamma ray detection efficiency of the prototype detector when compared to simulations performed in Geant4. To this end we have used three techniques to do a measurement of the gamma ray efficiency compared to simulation. The first is using electron capture sources that emit an X-ray before prompt emission of a de-excitation gamma ray, specifically Zn-65 and Mn-54. The second is using a beta + decay source wherein a positron annihilates on an atomic shell electron producing two back-to-back 511 keV gammas followed promptly by a de-excitation gamma, specifically Na-22. The third is using a gamma cascade of two near-simultaneous de-excitation gammas from the same nucleus, specifically from Co-60 decay.

physics.ins-det↗

arXiv2023

New lower background and higher rate technique for anti-neutrino detection using Tungsten 183 Isotope

Low energy anti-neutrinos detected from reactors or other sources have typically used the conversion of an anti-neutrino on Hydrogen, producing a positron and a free neutron. This neutron is subsequently captured on a secondary element with a large neutron capture cross section such as gadolinium or cadmium. We have studied the anti-neutrino conversion and suggest other elements that have a comparable cross section for anti-neutrino reactions. With most neutron captures on gadolinium, it is possible to get two or three delayed gamma signals of known energy to occur. Experiments like ATLAS can make measurements with timing on the order of 25 ns. With electronics like these, this leads to the possibility of having a triple delayed coincidence using the positron annihilation on atomic shell electrons as the starting signal. We have also found an isotope of tungsten, $^{183}$W that offers a large anti-neutrino interaction cross section of $1.19 \times 10^{-46}$ m$^2$ and an anti-neutrino threshold energy for the production of the ground state at 2.094 MeV and the production of the first excited state at 2.167 MeV. This reaction makes a nuclear m1 excited state of $^{183}$Ta$^*$ that emits a signature secondary gamma pulse of 73 keV with a 106 ns half-life. This offers a new delayed coincidence technique that can be used to identify anti-neutrinos with lower background noise. This allows for less shielding than required for modern inverse beta decay detectors.

physics.ins-det↗

arXiv2023

Estimating at Earth the Ultra-High Energy Neutrino Flux from the Accretion Disks in the Galactic Core

This research is to determine at Earth the high-energy neutrino flux coming from the galactic core, and from the many other accretion disks within the galactic core. It is estimated there are 10,000 such accretion disk within the cubic parsec of the galactic core alone and many more in the galactic core halo. There are various neutrino detectors, such as IceCube, which can detect energetic neutrinos. However, the direct galactic core neutrino flux is exceptionally low, so very few neutrinos from the galactic core are measured. We created two models to simulate the galactic core neutrino flux. To better estimate the neutrino flux we randomly distributed the accretion disks and generated bodies of varying sizes. This was then used to determine the ultra-high energy neutrino flux. Since it is extremely difficult to determine neutrino direction from interactions of neutrinos, we envision an application where the energetic galactic core neutrinos are gravitationally focused by the Sun with a large light collecting power of eleven to twelve orders of magnitude. They could interact in a planet's atmosphere where the produced showers containing energetic charged particles can produce Cherenkov rings imageable by an orbiting spacecraft or upward going muons which can be observed in a cosmic ray experiment. Estimating the flux will provide a general approximation of the number of ultra-high energy neutrinos that should reach Earth, with Earth being the overall detector. Moreover, studying the neutrinos will provide more information on the conditions of the galactic region, and allow characterizations of it to be formed.

astro-ph.HE↗

arXiv2022

A Possible Dark Matter Search Mission in Space

Direct detection of dark matter continues to elude scientists' many attempts to see it interact, and still to this day the only way we know it is there is through observed gravitational effects. The many search experiments are at the point where the search for dark matter direct observation is limited by the solar neutrino background signal here at Earth. Past experiments typically use a large volume central detector looking for energy materializing inside a detector volume that is not associated with any tracks of particles entering the volume through the surrounding active veto array and passive shielding. Here will be presented a new alternative method to see dark matter performing a search by changing the distance away from the Sun where the 1/r$^2$ law could be removed from the observations in a known predictable way. A Dark Matter detector on a spacecraft or built inside an asteroid might be possible. Many near Earth asteroids that can be easily reached by a spacecraft often have paths going in to the orbit of Venus and out to almost the orbit of Jupiter. These asteroids are made of ice, such as Crete, rubble piles of loosely bound boulders and pebbles, or a combination of the two. Landing on an asteroid where a space craft could melt its way under the surface for asteroids made mostly of ice or clawing its way into an asteroid could provide two advantages: shielding from cosmic and gamma rays and the ice that is melted to tunnel into the asteroid could become part of a much larger dark matter detector. Both of these advantages would allow a much larger dark matter detector than could have been brought with the spacecraft from Earth.

hep-ex↗

arXiv2022

Development of a neutrino detector capable of operating in space

The $\nu$SOL experiment to operate a neutrino detector close to the Sun is building a small test detector to orbit the Earth to test the concept in space. This detector concept is to provide a new way to detect neutrinos unshielded in space. A double delayed coincidence on Gallium nuclei that have a large cross section for solar neutrino interactions emitting a conversion electron and converting the nuclei into an excited state of Germanium, which decays with a well-known energy and half-life. This unique signature permits operation of the detector volume mostly unshielded in space with a high single particle counting rate from gamma and cosmic ray events. The test detector concept which has been studied in the lab and is planned for a year of operations orbiting Earth which is scheduled for launch in late 2024. It will be surrounded by an active veto and shielding will be operated in a polar orbit around the Earth to validate the detector concept and study detailed background spectrums that can fake the double timing and energy signature from random galactic cosmic or gamma rays. The success of this new technology development will permit the design of a larger spacecraft with a mission to fly close to the Sun and is of importance to the primary science mission of the Heliophysics division of NASA Space Science Mission Directorate, which is to better understand the Sun by measuring details of our Sun's fusion core.

hep-ex↗

arXiv2000

Latest Results on Weak Semi-Leptonic Hyperon Decays in KTeV

The KTeV experiment at Fermilab has finished its $Ξ^0$ semi-leptonic decay analysis from the 1997 run and presented here are the final numbers for the branching ratio and form factors. A new run with three times the statistics was taken in 1999 and a first look at the data shows the quality and consistency of the results, predicting a similar improvement in these measurements.

hep-ex↗