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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1805.06314">arXiv:1805.06314</a> <span> [<a href="https://arxiv.org/pdf/1805.06314">pdf</a>, <a href="https://arxiv.org/format/1805.06314">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Physics">physics.gen-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-018-6333-8">10.1140/epjc/s10052-018-6333-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Emission of cosmic rays from Jupiter. Magnetospheres as Sources of Cosmic Rays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Pizzella%2C+G">G. Pizzella</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1805.06314v2-abstract-short" style="display: inline;"> Measurements made recently with the PAMELA satellite have shown with good evidence that a fraction of the cosmic rays detected on Earth comes from Jupiter. This result draws attention to the idea that magnetospheres of astrophysical objects could contribute to the sources of cosmic rays. We discuss this conjecture on the basis of Earth installed instrumentation and of the measurements made with PA… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.06314v2-abstract-full').style.display = 'inline'; document.getElementById('1805.06314v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.06314v2-abstract-full" style="display: none;"> Measurements made recently with the PAMELA satellite have shown with good evidence that a fraction of the cosmic rays detected on Earth comes from Jupiter. This result draws attention to the idea that magnetospheres of astrophysical objects could contribute to the sources of cosmic rays. We discuss this conjecture on the basis of Earth installed instrumentation and of the measurements made with PAMELA. The experiments strongly favor the validity of the conjecture. In particular the PAMELA data show that the proton fluxes are larger when the Earth orbit intersects the lines of the interplanetary magnetic field connecting Jupiter with Earth. This effect shows up with more than ten standard deviations, difficult to explain without the idea that part of the cosmic ray protons comes directly from the Jupiter magnetosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.06314v2-abstract-full').style.display = 'none'; document.getElementById('1805.06314v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2018. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1801.08418">arXiv:1801.08418</a> <span> [<a href="https://arxiv.org/pdf/1801.08418">pdf</a>, <a href="https://arxiv.org/format/1801.08418">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/aaa403">10.3847/2041-8213/aaa403 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Unexpected cyclic behavior in cosmic ray protons observed by PAMELA at 1 AU </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Karelin%2C+A+V">A. V. Karelin</a>, <a href="/search/physics?searchtype=author&query=Koldashov%2C+S+V">S. V. Koldashov</a>, <a href="/search/physics?searchtype=author&query=Koldobskiy%2C+S">S. Koldobskiy</a>, <a href="/search/physics?searchtype=author&query=Krutkov%2C+S+Y">S. Y. Krutkov</a>, <a href="/search/physics?searchtype=author&query=Kvashnin%2C+A+N">A. N. Kvashnin</a>, <a href="/search/physics?searchtype=author&query=Leonov%2C+A">A. Leonov</a>, <a href="/search/physics?searchtype=author&query=Malakhov%2C+V">V. Malakhov</a>, <a href="/search/physics?searchtype=author&query=Marcelli%2C+L">L. Marcelli</a> , et al. (28 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1801.08418v1-abstract-short" style="display: inline;"> Protons detected by the PAMELA experiment in the period 2006-2014 have been analyzed in the energy range between 0.40-50 GV to explore possible periodicities besides the well known solar undecennial modulation. An unexpected clear and regular feature has been found at rigidities below 15 GV, with a quasi-periodicity of $\sim$450 days. A possible Jovian origin of this periodicity has been investiga… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.08418v1-abstract-full').style.display = 'inline'; document.getElementById('1801.08418v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.08418v1-abstract-full" style="display: none;"> Protons detected by the PAMELA experiment in the period 2006-2014 have been analyzed in the energy range between 0.40-50 GV to explore possible periodicities besides the well known solar undecennial modulation. An unexpected clear and regular feature has been found at rigidities below 15 GV, with a quasi-periodicity of $\sim$450 days. A possible Jovian origin of this periodicity has been investigated in different ways. The results seem to favor a small but not negligible contribution to cosmic rays from the Jovian magnetosphere, even if other explanations cannot be excluded. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.08418v1-abstract-full').style.display = 'none'; document.getElementById('1801.08418v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">article 4 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Letters, Volume 852, Number 2, 2018 January </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1604.06490">arXiv:1604.06490</a> <span> [<a href="https://arxiv.org/pdf/1604.06490">pdf</a>, <a href="https://arxiv.org/format/1604.06490">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="History and Philosophy of Physics">physics.hist-ph</span> </div> </div> <p class="title is-5 mathjax"> Personal recollections: Frascati and the search for gravitational waves at the Istituto Nazionale di Fisica Nucleare (INFN) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Pizzella%2C+G">Guido Pizzella</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1604.06490v1-abstract-short" style="display: inline;"> The history of the gravitational wave experiments at the Frascati National Laboratories of INFN is described, from the early suggestion of Edoardo Amaldi to the realization of NAUTILUS, the most sensitive detector at the end of the XXth century. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.06490v1-abstract-full" style="display: none;"> The history of the gravitational wave experiments at the Frascati National Laboratories of INFN is described, from the early suggestion of Edoardo Amaldi to the realization of NAUTILUS, the most sensitive detector at the end of the XXth century. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.06490v1-abstract-full').style.display = 'none'; document.getElementById('1604.06490v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> INFN-16-01/LNF </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1603.05076">arXiv:1603.05076</a> <span> [<a href="https://arxiv.org/pdf/1603.05076">pdf</a>, <a href="https://arxiv.org/format/1603.05076">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Physics">physics.gen-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> New analysis for the correlation between gravitational waves and neutrino detectors during SN1987A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Galeotti%2C+P">P. Galeotti</a>, <a href="/search/physics?searchtype=author&query=Pizzella%2C+G">G. Pizzella</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1603.05076v2-abstract-short" style="display: inline;"> Two major problems, still associated with the SN1987A, are: a) the signals observed with the gravitational waves detectors, b) the duration of the collapse. Indeed, a) the sensitivity of the gravitational wave detectors seems to be small for detecting gravitational waves and, b) while some experimental data indicate a duration of order of hours, most theories assume that the collapse develops in a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.05076v2-abstract-full').style.display = 'inline'; document.getElementById('1603.05076v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1603.05076v2-abstract-full" style="display: none;"> Two major problems, still associated with the SN1987A, are: a) the signals observed with the gravitational waves detectors, b) the duration of the collapse. Indeed, a) the sensitivity of the gravitational wave detectors seems to be small for detecting gravitational waves and, b) while some experimental data indicate a duration of order of hours, most theories assume that the collapse develops in a few seconds. Since recent data of the X-ray NuSTAR satellite show a clear evidence of an asymmetric collapse, we have revisited the experimental data recorded by the underground and gravitational wave detectors running during the SN1987A. New evidence is shown that con rms previous results, namely that the data recorded by the gravitational wave detectors running in Rome and in Maryland are strongly correlated with the data of both the Mont Blanc and the Kamiokande detectors, and that the correlation extends over a long period of time (one or two hours) centered at the Mont Blanc time. This result indicates that also Kamiokande detected neutrinos at the Mont Blanc time, and these interactions were not identi ed because not grouped in a burst. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.05076v2-abstract-full').style.display = 'none'; document.getElementById('1603.05076v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 6 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C (2016) 76-426 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1512.06249">arXiv:1512.06249</a> <span> [<a href="https://arxiv.org/pdf/1512.06249">pdf</a>, <a href="https://arxiv.org/format/1512.06249">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2015.12.007">10.1016/j.astropartphys.2015.12.007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dark Matter searches using gravitational wave bar detectors: quark nuggets and newtorites </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bassan%2C+M">M. Bassan</a>, <a href="/search/physics?searchtype=author&query=Coccia%2C+E">E. Coccia</a>, <a href="/search/physics?searchtype=author&query=D%27Antonio%2C+S">S. D'Antonio</a>, <a href="/search/physics?searchtype=author&query=Fafone%2C+V">V. Fafone</a>, <a href="/search/physics?searchtype=author&query=Giordano%2C+G">G. Giordano</a>, <a href="/search/physics?searchtype=author&query=Marini%2C+A">A. Marini</a>, <a href="/search/physics?searchtype=author&query=Minenkov%2C+Y">Y. Minenkov</a>, <a href="/search/physics?searchtype=author&query=Modena%2C+I">I. Modena</a>, <a href="/search/physics?searchtype=author&query=Pallottino%2C+G+V">G. V. Pallottino</a>, <a href="/search/physics?searchtype=author&query=Pizzella%2C+G">G. Pizzella</a>, <a href="/search/physics?searchtype=author&query=Rocchi%2C+A">A. Rocchi</a>, <a href="/search/physics?searchtype=author&query=Ronga%2C+F">F. Ronga</a>, <a href="/search/physics?searchtype=author&query=Visco%2C+M">M. Visco</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1512.06249v2-abstract-short" style="display: inline;"> Many experiments have searched for supersymmetric WIMP dark matter, with null results. This may suggest to look for more exotic possibilities, for example compact ultra-dense quark nuggets, widely discussed in literature with several different names. Nuclearites are an example of candidate compact objects with atomic size cross section. After a short discussion on nuclearites, the result of a nucl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.06249v2-abstract-full').style.display = 'inline'; document.getElementById('1512.06249v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1512.06249v2-abstract-full" style="display: none;"> Many experiments have searched for supersymmetric WIMP dark matter, with null results. This may suggest to look for more exotic possibilities, for example compact ultra-dense quark nuggets, widely discussed in literature with several different names. Nuclearites are an example of candidate compact objects with atomic size cross section. After a short discussion on nuclearites, the result of a nuclearite search with the gravitational wave bar detectors Nautilus and Explorer is reported. The geometrical acceptance of the bar detectors is 19.5 $\rm m^2$ sr, that is smaller than that of other detectors used for similar searches. However, the detection mechanism is completely different and is more straightforward than in other detectors. The experimental limits we obtain are of interest because, for nuclearites of mass less than $10^{-5}$ g, we find a flux smaller than that one predicted considering nuclearites as dark matter candidates. Particles with gravitational only interactions (newtorites) are another example. In this case the sensitivity is quite poor and a short discussion is reported on possible improvements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.06249v2-abstract-full').style.display = 'none'; document.getElementById('1512.06249v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">published on Astroparticle Physics Sept 25th 2016 replaced fig 15</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1306.5164">arXiv:1306.5164</a> <span> [<a href="https://arxiv.org/pdf/1306.5164">pdf</a>, <a href="https://arxiv.org/format/1306.5164">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Quark nuggets search using 2350 Kg gravitational waves aluminum bar detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Astone%2C+P">P. Astone</a>, <a href="/search/physics?searchtype=author&query=Bassan%2C+M">M. Bassan</a>, <a href="/search/physics?searchtype=author&query=Coccia%2C+E">E. Coccia</a>, <a href="/search/physics?searchtype=author&query=D%27Antonio%2C+S">S. D'Antonio</a>, <a href="/search/physics?searchtype=author&query=Fafone%2C+V">V. Fafone</a>, <a href="/search/physics?searchtype=author&query=Giordano%2C+G">G. Giordano</a>, <a href="/search/physics?searchtype=author&query=Marini%2C+A">A. Marini</a>, <a href="/search/physics?searchtype=author&query=Minenkov%2C+Y">Y. Minenkov</a>, <a href="/search/physics?searchtype=author&query=Modena%2C+I">I. Modena</a>, <a href="/search/physics?searchtype=author&query=Moleti%2C+A">A. Moleti</a>, <a href="/search/physics?searchtype=author&query=Pallottino%2C+G+V">G. V. Pallottino</a>, <a href="/search/physics?searchtype=author&query=Pizzella%2C+G">G. Pizzella</a>, <a href="/search/physics?searchtype=author&query=Rocchi%2C+A">A. Rocchi</a>, <a href="/search/physics?searchtype=author&query=Ronga%2C+F">F. Ronga</a>, <a href="/search/physics?searchtype=author&query=Visco%2C+M">M. Visco</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1306.5164v1-abstract-short" style="display: inline;"> The gravitational wave resonant detectors can be used as detectors of quark nuggets, like nuclearites (nuclear matter with a strange quark). This search has been carried out using data from two 2350 Kg, 2 K cooled, aluminum bar detectors: NAUTILUS, located in Frascati (Italy), and EXPLORER, that was located in CERN Geneva (CH). Both antennas are equipped with cosmic ray shower detectors: signals i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1306.5164v1-abstract-full').style.display = 'inline'; document.getElementById('1306.5164v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1306.5164v1-abstract-full" style="display: none;"> The gravitational wave resonant detectors can be used as detectors of quark nuggets, like nuclearites (nuclear matter with a strange quark). This search has been carried out using data from two 2350 Kg, 2 K cooled, aluminum bar detectors: NAUTILUS, located in Frascati (Italy), and EXPLORER, that was located in CERN Geneva (CH). Both antennas are equipped with cosmic ray shower detectors: signals in the bar due to showers are continuously detected and used to characterize the antenna performances. The bar excitation mechanism is based on the so called thermo-acoustic effect, studied on dedicated experiments that use particle beams. This mechanism predicts that vibrations of bars are induced by the heat deposited in the bar from the particle. The geometrical acceptance of the bar detectors is 19.5 $\rm m^2$ sr, that is smaller than that of other detectors used for similar searches. However, the detection mechanism is completely different and is more straightforward than in other detectors. We will show the results of ten years of data from NAUTILUS (2003-2012) and 7 years from EXPLORER (2003-2009). The experimental limits we obtain are of interest because, for nuclearites of mass less than $10^{-4}$ grams, we find a flux smaller than that one predicted considering nuclearites as dark matter candidates. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1306.5164v1-abstract-full').style.display = 'none'; document.getElementById('1306.5164v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 June, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">presented to the 33rd International Cosmic Ray Conference Rio de Janeiro 2013</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1211.2913">arXiv:1211.2913</a> <span> [<a href="https://arxiv.org/pdf/1211.2913">pdf</a>, <a href="https://arxiv.org/format/1211.2913">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Accelerator Physics">physics.acc-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Physics">physics.gen-ph</span> </div> </div> <p class="title is-5 mathjax"> Measuring Propagation Speed of Coulomb Fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=de+Sangro%2C+R">R. de Sangro</a>, <a href="/search/physics?searchtype=author&query=Finocchiaro%2C+G">G. Finocchiaro</a>, <a href="/search/physics?searchtype=author&query=Patteri%2C+P">P. Patteri</a>, <a href="/search/physics?searchtype=author&query=Piccolo%2C+M">M. Piccolo</a>, <a href="/search/physics?searchtype=author&query=Pizzella%2C+G">G. Pizzella</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1211.2913v2-abstract-short" style="display: inline;"> The problem of gravity propagation has been subject of discussion for quite a long time: Newton, Laplace and, in relatively more modern times, Eddington pointed out that, if gravity propagated with finite velocity, planets motion around the sun would become unstable due to a torque originating from time lag of the gravitational interactions. Such an odd behavior can be found also in electromagne… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.2913v2-abstract-full').style.display = 'inline'; document.getElementById('1211.2913v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1211.2913v2-abstract-full" style="display: none;"> The problem of gravity propagation has been subject of discussion for quite a long time: Newton, Laplace and, in relatively more modern times, Eddington pointed out that, if gravity propagated with finite velocity, planets motion around the sun would become unstable due to a torque originating from time lag of the gravitational interactions. Such an odd behavior can be found also in electromagnetism, when one computes the propagation of the electric fields generated by a set of uniformly moving charges. As a matter of fact the Li茅nard-Weichert retarded potential leads to a formula indistinguishable from the one obtained assuming that the electric field propagates with infinite velocity. Feyman explanation for this apparent paradox was based on the fact that uniform motions last indefinitely. To verify such an explanation, we performed an experiment to measure the time/space evolution of the electric field generated by an uniformely moving electron beam. The results we obtain on such a finite lifetime kinematical state seem compatible with an electric field rigidly carried by the beam itself. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.2913v2-abstract-full').style.display = 'none'; document.getElementById('1211.2913v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 November, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 November, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 15 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1105.4724">arXiv:1105.4724</a> <span> [<a href="https://arxiv.org/pdf/1105.4724">pdf</a>, <a href="https://arxiv.org/format/1105.4724">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2011.08.028">10.1016/j.nima.2011.08.028 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Vibrational excitation induced by electron beam and cosmic rays in normal and superconductive aluminum bars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bassan%2C+M">M. Bassan</a>, <a href="/search/physics?searchtype=author&query=Buonomo%2C+B">B. Buonomo</a>, <a href="/search/physics?searchtype=author&query=Cavallari%2C+G">G. Cavallari</a>, <a href="/search/physics?searchtype=author&query=Coccia%2C+E">E. Coccia</a>, <a href="/search/physics?searchtype=author&query=D%27Antonio%2C+S">S. D'Antonio</a>, <a href="/search/physics?searchtype=author&query=Fafone%2C+V">V. Fafone</a>, <a href="/search/physics?searchtype=author&query=Foggetta%2C+L+G">L. G. Foggetta</a>, <a href="/search/physics?searchtype=author&query=Ligi%2C+C">C. Ligi</a>, <a href="/search/physics?searchtype=author&query=Marini%2C+A">A. Marini</a>, <a href="/search/physics?searchtype=author&query=Mazzitelli%2C+G">G. Mazzitelli</a>, <a href="/search/physics?searchtype=author&query=Modestino%2C+G">G. Modestino</a>, <a href="/search/physics?searchtype=author&query=Pizzella%2C+G">G. Pizzella</a>, <a href="/search/physics?searchtype=author&query=Quintieri%2C+L">L. Quintieri</a>, <a href="/search/physics?searchtype=author&query=Ronga%2C+F">F. Ronga</a>, <a href="/search/physics?searchtype=author&query=Valente%2C+P">P. Valente</a>, <a href="/search/physics?searchtype=author&query=Vinko%2C+S+M">S. M. Vinko</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1105.4724v2-abstract-short" style="display: inline;"> We report new measurements of the acoustic excitation of an Al5056 superconductive bar when hit by an electron beam, in a previously unexplored temperature range, down to 0.35 K. These data, analyzed together with previous results of the RAP experiment obtained for T > 0.54 K, show a vibrational response enhanced by a factor 4.9 with respect to that measured in the normal state. This enhancement e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1105.4724v2-abstract-full').style.display = 'inline'; document.getElementById('1105.4724v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1105.4724v2-abstract-full" style="display: none;"> We report new measurements of the acoustic excitation of an Al5056 superconductive bar when hit by an electron beam, in a previously unexplored temperature range, down to 0.35 K. These data, analyzed together with previous results of the RAP experiment obtained for T > 0.54 K, show a vibrational response enhanced by a factor 4.9 with respect to that measured in the normal state. This enhancement explains the anomalous large signals due to cosmic rays previously detected in the NAUTILUS gravitational wave detector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1105.4724v2-abstract-full').style.display = 'none'; document.getElementById('1105.4724v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 August, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 May, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 13 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0901.1220">arXiv:0901.1220</a> <span> [<a href="https://arxiv.org/pdf/0901.1220">pdf</a>, <a href="https://arxiv.org/format/0901.1220">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.physleta.2009.03.043">10.1016/j.physleta.2009.03.043 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Experimental study of high energy electron interactions in a superconducting aluminum alloy resonant bar </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Barucci%2C+M">M. Barucci</a>, <a href="/search/physics?searchtype=author&query=Bassan%2C+M">M. Bassan</a>, <a href="/search/physics?searchtype=author&query=Buonomo%2C+B">B. Buonomo</a>, <a href="/search/physics?searchtype=author&query=Cavallari%2C+G">G. Cavallari</a>, <a href="/search/physics?searchtype=author&query=Coccia%2C+E">E. Coccia</a>, <a href="/search/physics?searchtype=author&query=D%27Antonio%2C+S">S. D'Antonio</a>, <a href="/search/physics?searchtype=author&query=Fafone%2C+V">V. Fafone</a>, <a href="/search/physics?searchtype=author&query=Ligi%2C+C">C. Ligi</a>, <a href="/search/physics?searchtype=author&query=Lolli%2C+L">L. Lolli</a>, <a href="/search/physics?searchtype=author&query=Marini%2C+A">A. Marini</a>, <a href="/search/physics?searchtype=author&query=Mazzitelli%2C+G">G. Mazzitelli</a>, <a href="/search/physics?searchtype=author&query=Modestino%2C+G">G. Modestino</a>, <a href="/search/physics?searchtype=author&query=Pizzella%2C+G">G. Pizzella</a>, <a href="/search/physics?searchtype=author&query=Quintieri%2C+L">L. Quintieri</a>, <a href="/search/physics?searchtype=author&query=Risegari%2C+L">L. Risegari</a>, <a href="/search/physics?searchtype=author&query=Rocchi%2C+A">A. Rocchi</a>, <a href="/search/physics?searchtype=author&query=Ronga%2C+F">F. Ronga</a>, <a href="/search/physics?searchtype=author&query=Valente%2C+P">P. Valente</a>, <a href="/search/physics?searchtype=author&query=Ventura%2C+G">G. Ventura</a>, <a href="/search/physics?searchtype=author&query=Vinko%2C+S+M">S. M. Vinko</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0901.1220v1-abstract-short" style="display: inline;"> Peak amplitude measurements of the fundamental mode of oscillation of a suspended aluminum alloy bar hit by an electron beam show that the amplitude is enhanced by a factor ~3.5 when the material is in the superconducting state. This result is consistent with the cosmic ray observations made by the resonant gravitational wave detector NAUTILUS, made of the same alloy, when operated in the superc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0901.1220v1-abstract-full').style.display = 'inline'; document.getElementById('0901.1220v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0901.1220v1-abstract-full" style="display: none;"> Peak amplitude measurements of the fundamental mode of oscillation of a suspended aluminum alloy bar hit by an electron beam show that the amplitude is enhanced by a factor ~3.5 when the material is in the superconducting state. This result is consistent with the cosmic ray observations made by the resonant gravitational wave detector NAUTILUS, made of the same alloy, when operated in the superconducting state. A comparison of the experimental data with the predictions of the model describing the underlying physical process is also presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0901.1220v1-abstract-full').style.display = 'none'; document.getElementById('0901.1220v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 January, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Lett.A373:1801-1806,2009 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0809.3670">arXiv:0809.3670</a> <span> [<a href="https://arxiv.org/pdf/0809.3670">pdf</a>, <a href="https://arxiv.org/ps/0809.3670">ps</a>, <a href="https://arxiv.org/format/0809.3670">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Classical Physics">physics.class-ph</span> </div> </div> <p class="title is-5 mathjax"> On Cosmic Rays Sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Pizzella%2C+G">G. Pizzella</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0809.3670v1-abstract-short" style="display: inline;"> Study of astrophysical objects with strong dipolar magnetic fields show that the spectrum of the accelerated charged particles leaving the sources has a power law form with exponent -2.5, where the exponent is calculated on purely geometrical bases and is independent on the particle species. </span> <span class="abstract-full has-text-grey-dark mathjax" id="0809.3670v1-abstract-full" style="display: none;"> Study of astrophysical objects with strong dipolar magnetic fields show that the spectrum of the accelerated charged particles leaving the sources has a power law form with exponent -2.5, where the exponent is calculated on purely geometrical bases and is independent on the particle species. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0809.3670v1-abstract-full').style.display = 'none'; document.getElementById('0809.3670v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 September, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2008. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0206431">arXiv:astro-ph/0206431</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0206431">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0206431">ps</a>, <a href="https://arxiv.org/format/astro-ph/0206431">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.66.102002">10.1103/PhysRevD.66.102002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for correlation between GRB's detected by BeppoSAX and gravitational wave detectors EXPLORER and NAUTILUS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Astone%2C+P">P. Astone</a>, <a href="/search/physics?searchtype=author&query=Bassan%2C+M">M. Bassan</a>, <a href="/search/physics?searchtype=author&query=Bonifazi%2C+P">P. Bonifazi</a>, <a href="/search/physics?searchtype=author&query=Carelli%2C+P">P. Carelli</a>, <a href="/search/physics?searchtype=author&query=Castellano%2C+G">G. Castellano</a>, <a href="/search/physics?searchtype=author&query=Coccia%2C+E">E. Coccia</a>, <a href="/search/physics?searchtype=author&query=Cosmelli%2C+C">C. Cosmelli</a>, <a href="/search/physics?searchtype=author&query=D%27Agostini%2C+G">G. D'Agostini</a>, <a href="/search/physics?searchtype=author&query=D%27Antonio%2C+S">S. D'Antonio</a>, <a href="/search/physics?searchtype=author&query=Fafone%2C+V">V. Fafone</a>, <a href="/search/physics?searchtype=author&query=Federici%2C+G">G. Federici</a>, <a href="/search/physics?searchtype=author&query=Frontera%2C+F">F. Frontera</a>, <a href="/search/physics?searchtype=author&query=Guidorzi%2C+C">C. Guidorzi</a>, <a href="/search/physics?searchtype=author&query=Marini%2C+A">A. Marini</a>, <a href="/search/physics?searchtype=author&query=Minenkov%2C+Y">Y. Minenkov</a>, <a href="/search/physics?searchtype=author&query=Modena%2C+I">I. Modena</a>, <a href="/search/physics?searchtype=author&query=Modestino%2C+G">G. Modestino</a>, <a href="/search/physics?searchtype=author&query=Moleti%2C+A">A. Moleti</a>, <a href="/search/physics?searchtype=author&query=Montanari%2C+E">E. Montanari</a>, <a href="/search/physics?searchtype=author&query=Pallottino%2C+G+V">G. V. Pallottino</a>, <a href="/search/physics?searchtype=author&query=Pizzella%2C+G">G. Pizzella</a>, <a href="/search/physics?searchtype=author&query=Quintieri%2C+L">L. Quintieri</a>, <a href="/search/physics?searchtype=author&query=Rocchi%2C+A">A. Rocchi</a>, <a href="/search/physics?searchtype=author&query=Ronga%2C+F">F. Ronga</a>, <a href="/search/physics?searchtype=author&query=Rocchi%2C+A">A. Rocchi</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0206431v2-abstract-short" style="display: inline;"> Data obtained during five months of 2001 with the gravitational wave (GW) detectors EXPLORER and NAUTILUS were studied in correlation with the gamma ray burst data (GRB) obtained with the BeppoSAX satellite. During this period BeppoSAX was the only GRB satellite in operation, while EXPLORER and NAUTILUS were the only GW detectors in operation. No correlation between the GW data and the GRB bur… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0206431v2-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0206431v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0206431v2-abstract-full" style="display: none;"> Data obtained during five months of 2001 with the gravitational wave (GW) detectors EXPLORER and NAUTILUS were studied in correlation with the gamma ray burst data (GRB) obtained with the BeppoSAX satellite. During this period BeppoSAX was the only GRB satellite in operation, while EXPLORER and NAUTILUS were the only GW detectors in operation. No correlation between the GW data and the GRB bursts was found. The analysis, performed over 47 GRB's, excludes the presence of signals of amplitude h >=1.2 * 10^{-18}, with 95 % probability, if we allow a time delay between GW bursts and GRB within +-400 s, and h >= 6.5 * 10^{-19}, if the time delay is within +- 5 s. The result is also provided in form of scaled likelihood for unbiased interpretation and easier use for further analysis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0206431v2-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0206431v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 July, 2002; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 June, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2002. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 7 figures. Latex file, compiled with cernik.cls (provided in the package)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev. D66 (2002) 102002 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-ex/0002028">arXiv:hep-ex/0002028</a> <span> [<a href="https://arxiv.org/pdf/hep-ex/0002028">pdf</a>, <a href="https://arxiv.org/ps/hep-ex/0002028">ps</a>, <a href="https://arxiv.org/format/hep-ex/0002028">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> </div> </div> <p class="title is-5 mathjax"> Upper Limits in the Case That Zero Events are Observed: An Intuitive Solution to the Background Dependence Puzzle </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Astone%2C+P">P. Astone</a>, <a href="/search/physics?searchtype=author&query=Pizzella%2C+G">G. Pizzella</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="hep-ex/0002028v1-abstract-short" style="display: inline;"> We compare the ``unified approach'' for the estimation of upper limits with an approach based on the Bayes theory, in the special case that no events are observed. The ``unified approach'' predicts, in this case, an upper limit that decreases with the increase in the expected level of background. This seems absurd. On the other hand, the Bayesian approach leads to a result which is background in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0002028v1-abstract-full').style.display = 'inline'; document.getElementById('hep-ex/0002028v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-ex/0002028v1-abstract-full" style="display: none;"> We compare the ``unified approach'' for the estimation of upper limits with an approach based on the Bayes theory, in the special case that no events are observed. The ``unified approach'' predicts, in this case, an upper limit that decreases with the increase in the expected level of background. This seems absurd. On the other hand, the Bayesian approach leads to a result which is background independent. An explanation of the Bayesian result is presented, together with suggested reasons for the paradoxical result of the ``unified approach''. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0002028v1-abstract-full').style.display = 'none'; document.getElementById('hep-ex/0002028v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 February, 2000; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2000. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Latex file (compiled with cernrep.cls included) 5 pages, no figures. To appear in the Proceed. of the workshop on ''Confidence limits'' (CERN, Jan 2000). This paper and related papers also available at http://grwav3.roma1.infn.it/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/gr-qc/0001035">arXiv:gr-qc/0001035</a> <span> [<a href="https://arxiv.org/pdf/gr-qc/0001035">pdf</a>, <a href="https://arxiv.org/ps/gr-qc/0001035">ps</a>, <a href="https://arxiv.org/format/gr-qc/0001035">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Probability">math.PR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/S0927-6505(01)00166-9">10.1016/S0927-6505(01)00166-9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On Upper Limits for Gravitational Radiation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Astone%2C+P">P. Astone</a>, <a href="/search/physics?searchtype=author&query=Pizzella%2C+G">G. Pizzella</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="gr-qc/0001035v2-abstract-short" style="display: inline;"> A procedure with a Bayesan approach for calculating upper limits to gravitational wave bursts from coincidence experiments with multiple detectors is described. </span> <span class="abstract-full has-text-grey-dark mathjax" id="gr-qc/0001035v2-abstract-full" style="display: none;"> A procedure with a Bayesan approach for calculating upper limits to gravitational wave bursts from coincidence experiments with multiple detectors is described. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('gr-qc/0001035v2-abstract-full').style.display = 'none'; document.getElementById('gr-qc/0001035v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 January, 2000; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 January, 2000; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2000. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 2 figures, latex files using cernlik.cls (included). This paper and related work are also available at http://grwav3.roma1.infn.it/pia/papersweb.html Version number 2: text unchanged. Modified two references, adding the hep numbers</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astropart.Phys.16:441-450,2002 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 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