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<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/2110.05135">arXiv:2110.05135</a> <span> [<a href="https://arxiv.org/pdf/2110.05135">pdf</a>, <a href="https://arxiv.org/format/2110.05135">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="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> Dark gravitomagnetism with LISA and gravitational waves space detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Tartaglia%2C+A">Angelo Tartaglia</a>, <a href="/search/physics?searchtype=author&query=Bassan%2C+M">Massimo Bassan</a>, <a href="/search/physics?searchtype=author&query=Pucacco%2C+G">Giuseppe Pucacco</a>, <a href="/search/physics?searchtype=author&query=Ferroni%2C+V">Valerio Ferroni</a>, <a href="/search/physics?searchtype=author&query=Vetrugno%2C+D">Daniele Vetrugno</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="2110.05135v1-abstract-short" style="display: inline;"> We present here the proposal to use the LISA interferometer for detecting the gravito-magnetic field due to the rotation of the Milky Way, including the contribution given by the dark matter halo. The galactic signal would be superposed to the gravitomagnetic field of the Sun. The technique to be used is based on the asymmetric propagation of light along the closed contour of the space interferome… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.05135v1-abstract-full').style.display = 'inline'; document.getElementById('2110.05135v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.05135v1-abstract-full" style="display: none;"> We present here the proposal to use the LISA interferometer for detecting the gravito-magnetic field due to the rotation of the Milky Way, including the contribution given by the dark matter halo. The galactic signal would be superposed to the gravitomagnetic field of the Sun. The technique to be used is based on the asymmetric propagation of light along the closed contour of the space interferometer (Sagnac-like approach). Both principle and practical aspects of the proposed experiment are discussed. The strategy for disentangling the sought for signal from the kinematic terms due to proper rotation and orbital motion is based on the time modulation of the time of flight asymmetry. Such modulation will be originated by the annual oscillation of the plane of the interferometer with respect to the galactic plane. Also the effect of the gravitomagnetic field on the polarization of the electromagnetic signals is presented as an in principle detectable phenomenon. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.05135v1-abstract-full').style.display = 'none'; document.getElementById('2110.05135v1-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> 11 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </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">13, 2 figures, to be published in the Proceedings of the 16th Marcel Grossmann meeting (2021)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.12855">arXiv:1904.12855</a> <span> [<a href="https://arxiv.org/pdf/1904.12855">pdf</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="Classical Physics">physics.class-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/10.1142/S0218271819501153">10.1142/S0218271819501153 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Liquid actuated gravity experiments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bassan%2C+M">Massimo Bassan</a>, <a href="/search/physics?searchtype=author&query=De+Laurentis%2C+M">Martina De Laurentis</a>, <a href="/search/physics?searchtype=author&query=De+Rosa%2C+R">Rosario De Rosa</a>, <a href="/search/physics?searchtype=author&query=Di+Fiore%2C+L">Luciano Di Fiore</a>, <a href="/search/physics?searchtype=author&query=Errico%2C+L">Luciano Errico</a>, <a href="/search/physics?searchtype=author&query=Garufi%2C+F">Fabio Garufi</a>, <a href="/search/physics?searchtype=author&query=Grado%2C+A">Aniello Grado</a>, <a href="/search/physics?searchtype=author&query=Minenkov%2C+Y">Yury Minenkov</a>, <a href="/search/physics?searchtype=author&query=Pucacco%2C+G">Giuseppe Pucacco</a>, <a href="/search/physics?searchtype=author&query=Visco%2C+M">Massimo 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="1904.12855v1-abstract-short" style="display: inline;"> We describe a new actuation technique for gravity experiments based on a liquid field mass. The Characterizing idea is to modulate the gravity force acting on a test mass by controlling the level of a liquid in a suitable container. This allows to obtain a periodical gravity force without moving parts (except the liquid level) close to the TM. We describe in detail the most relevant aspects of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.12855v1-abstract-full').style.display = 'inline'; document.getElementById('1904.12855v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.12855v1-abstract-full" style="display: none;"> We describe a new actuation technique for gravity experiments based on a liquid field mass. The Characterizing idea is to modulate the gravity force acting on a test mass by controlling the level of a liquid in a suitable container. This allows to obtain a periodical gravity force without moving parts (except the liquid level) close to the TM. We describe in detail the most relevant aspects of the liquid actuator and discuss how it can be used in gravity experiments. In particular we analyse an application to test the inverse square law in the mm to cm distance region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.12855v1-abstract-full').style.display = 'none'; document.getElementById('1904.12855v1-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 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.09374">arXiv:1802.09374</a> <span> [<a href="https://arxiv.org/pdf/1802.09374">pdf</a>, <a href="https://arxiv.org/ps/1802.09374">ps</a>, <a href="https://arxiv.org/format/1802.09374">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.3847/1538-4357/aaa774">10.3847/1538-4357/aaa774 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characteristics and energy dependence of recurrent galactic cosmic-ray flux depressions and of a Forbush decrease with LISA Pathfinder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Armano%2C+M">M. Armano</a>, <a href="/search/physics?searchtype=author&query=Audley%2C+H">H. Audley</a>, <a href="/search/physics?searchtype=author&query=Baird%2C+J">J. Baird</a>, <a href="/search/physics?searchtype=author&query=Bassan%2C+M">M. Bassan</a>, <a href="/search/physics?searchtype=author&query=Benella%2C+S">S. Benella</a>, <a href="/search/physics?searchtype=author&query=Binetruy%2C+P">P. Binetruy</a>, <a href="/search/physics?searchtype=author&query=Born%2C+M">M. Born</a>, <a href="/search/physics?searchtype=author&query=Bortoluzzi%2C+D">D. Bortoluzzi</a>, <a href="/search/physics?searchtype=author&query=Cavalleri%2C+A">A. Cavalleri</a>, <a href="/search/physics?searchtype=author&query=Cesarini%2C+A">A. Cesarini</a>, <a href="/search/physics?searchtype=author&query=Cruise%2C+A+M">A. M. Cruise</a>, <a href="/search/physics?searchtype=author&query=Danzmann%2C+K">K. Danzmann</a>, <a href="/search/physics?searchtype=author&query=Silva%2C+M+d+D">M. de Deus Silva</a>, <a href="/search/physics?searchtype=author&query=Diepholz%2C+I">I. Diepholz</a>, <a href="/search/physics?searchtype=author&query=Dixon%2C+G">G. Dixon</a>, <a href="/search/physics?searchtype=author&query=Dolesi%2C+R">R. Dolesi</a>, <a href="/search/physics?searchtype=author&query=Fabi%2C+M">M. Fabi</a>, <a href="/search/physics?searchtype=author&query=Ferraioli%2C+L">L. Ferraioli</a>, <a href="/search/physics?searchtype=author&query=Ferroni%2C+V">V. Ferroni</a>, <a href="/search/physics?searchtype=author&query=Finetti%2C+N">N. Finetti</a>, <a href="/search/physics?searchtype=author&query=Fitzsimons%2C+E+D">E. D. Fitzsimons</a>, <a href="/search/physics?searchtype=author&query=Freschi%2C+M">M. Freschi</a>, <a href="/search/physics?searchtype=author&query=Gesa%2C+L">L. Gesa</a>, <a href="/search/physics?searchtype=author&query=Gibert%2C+F">F. Gibert</a>, <a href="/search/physics?searchtype=author&query=Giardini%2C+D">D. Giardini</a> , et al. (60 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="1802.09374v2-abstract-short" style="display: inline;"> Galactic cosmic-ray (GCR) energy spectra observed in the inner heliosphere are modulated by the solar activity, the solar polarity and structures of solar and interplanetary origin. A high counting rate particle detector (PD) aboard LISA Pathfinder (LPF), meant for subsystems diagnostics, was devoted to the measurement of galactic cosmic-ray and solar energetic particle integral fluxes above 70 Me… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.09374v2-abstract-full').style.display = 'inline'; document.getElementById('1802.09374v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.09374v2-abstract-full" style="display: none;"> Galactic cosmic-ray (GCR) energy spectra observed in the inner heliosphere are modulated by the solar activity, the solar polarity and structures of solar and interplanetary origin. A high counting rate particle detector (PD) aboard LISA Pathfinder (LPF), meant for subsystems diagnostics, was devoted to the measurement of galactic cosmic-ray and solar energetic particle integral fluxes above 70 MeV n$^{-1}$ up to 6500 counts s$^{-1}$. PD data were gathered with a sampling time of 15 s. Characteristics and energy-dependence of GCR flux recurrent depressions and of a Forbush decrease dated August 2, 2016 are reported here. The capability of interplanetary missions, carrying PDs for instrument performance purposes, in monitoring the passage of interplanetary coronal mass ejections (ICMEs) is also discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.09374v2-abstract-full').style.display = 'none'; document.getElementById('1802.09374v2-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> 27 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, 854, 2018, 113 </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/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/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> </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 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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