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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/1608.03512">arXiv:1608.03512</a> <span> [<a href="https://arxiv.org/pdf/1608.03512">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Atomic Physics">physics.atom-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-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/10.1103/PhysRevLett.117.249501">10.1103/PhysRevLett.117.249501 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Comment on "Large enhancement in high-energy photoionization of Fe XVII and missing continuum plasma opacity" </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Blancard%2C+C">C. Blancard</a>, <a href="/search/physics?searchtype=author&query=Colgan%2C+J">J. Colgan</a>, <a href="/search/physics?searchtype=author&query=Coss%C3%A9%2C+P">Ph. Coss茅</a>, <a href="/search/physics?searchtype=author&query=Faussurier%2C+G">G. Faussurier</a>, <a href="/search/physics?searchtype=author&query=Fontes%2C+C+J">C. J. Fontes</a>, <a href="/search/physics?searchtype=author&query=Gilleron%2C+F">F. Gilleron</a>, <a href="/search/physics?searchtype=author&query=Golovkin%2C+I">I. Golovkin</a>, <a href="/search/physics?searchtype=author&query=Hansen%2C+S+B">S. B. Hansen</a>, <a href="/search/physics?searchtype=author&query=Iglesias%2C+C+A">C. A. Iglesias</a>, <a href="/search/physics?searchtype=author&query=Kilcrease%2C+D+P">D. P. Kilcrease</a>, <a href="/search/physics?searchtype=author&query=MacFarlane%2C+J+J">J. J. MacFarlane</a>, <a href="/search/physics?searchtype=author&query=More%2C+R+M">R. M. More</a>, <a href="/search/physics?searchtype=author&query=Pain%2C+J+-">J. -C. Pain</a>, <a href="/search/physics?searchtype=author&query=Sherrill%2C+M">M. Sherrill</a>, <a href="/search/physics?searchtype=author&query=Wilson%2C+B+G">B. G. Wilson</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="1608.03512v1-abstract-short" style="display: inline;"> Recent R-matrix calculations claim to produce a significant enhancement in the opacity of Fe XVII due to atomic core excitations [S. N. Nahar & A.K. Pradhan, Phys. Rev. Letters 116, 235003 (2016), arXiv:1606.02731] and assert that this enhancement is consistent with recent measurements of higher-than-predicted iron opacities [J. E. Bailey et al., Nature 517, 56 (2015)]. This comment shows that the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.03512v1-abstract-full').style.display = 'inline'; document.getElementById('1608.03512v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1608.03512v1-abstract-full" style="display: none;"> Recent R-matrix calculations claim to produce a significant enhancement in the opacity of Fe XVII due to atomic core excitations [S. N. Nahar & A.K. Pradhan, Phys. Rev. Letters 116, 235003 (2016), arXiv:1606.02731] and assert that this enhancement is consistent with recent measurements of higher-than-predicted iron opacities [J. E. Bailey et al., Nature 517, 56 (2015)]. This comment shows that the standard opacity models which have already been directly compared with experimental data produce photon absorption cross-sections for Fe XVII that are effectively equivalent to (and in fact larger than) the new R-matrix opacities. Thus, the new R-matrix results cannot be expected to significantly impact the existing discrepancies between theory and experiment because they produce neither a "large enhancement" nor account for "missing continuum plasma opacity" relative to standard models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.03512v1-abstract-full').style.display = 'none'; document.getElementById('1608.03512v1-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 August, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">three pages, one table, one figure</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1201.6245">arXiv:1201.6245</a> <span> [<a href="https://arxiv.org/pdf/1201.6245">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Atomic Physics">physics.atom-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-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/10.1016/j.hedp.2011.06.001">10.1016/j.hedp.2011.06.001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Comparison of Fe and Ni opacity calculations for a better understanding of pulsating stellar envelopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Gilles%2C+D">D. Gilles</a>, <a href="/search/physics?searchtype=author&query=Turck-Chi%C3%A8ze%2C+S">S. Turck-Chi猫ze</a>, <a href="/search/physics?searchtype=author&query=Loisel%2C+G">G. Loisel</a>, <a href="/search/physics?searchtype=author&query=Piau%2C+L">L. Piau</a>, <a href="/search/physics?searchtype=author&query=Ducret%2C+J+-">J. -E. Ducret</a>, <a href="/search/physics?searchtype=author&query=Poirier%2C+M">M. Poirier</a>, <a href="/search/physics?searchtype=author&query=Blenski%2C+T">T. Blenski</a>, <a href="/search/physics?searchtype=author&query=Thais%2C+F">F. Thais</a>, <a href="/search/physics?searchtype=author&query=Blancard%2C+C">C. Blancard</a>, <a href="/search/physics?searchtype=author&query=Coss%C3%A9%2C+P">P. Coss茅</a>, <a href="/search/physics?searchtype=author&query=Faussurier%2C+G">G. Faussurier</a>, <a href="/search/physics?searchtype=author&query=Gilleron%2C+F">F. Gilleron</a>, <a href="/search/physics?searchtype=author&query=Pain%2C+J+-">J. -C. Pain</a>, <a href="/search/physics?searchtype=author&query=Porcherot%2C+Q">Q. Porcherot</a>, <a href="/search/physics?searchtype=author&query=Guzik%2C+J+A">J. A. Guzik</a>, <a href="/search/physics?searchtype=author&query=Kilcrease%2C+D+P">D. P. Kilcrease</a>, <a href="/search/physics?searchtype=author&query=Magee%2C+N+H">N. H. Magee</a>, <a href="/search/physics?searchtype=author&query=Harris%2C+J">J. Harris</a>, <a href="/search/physics?searchtype=author&query=Busquet%2C+M">M. Busquet</a>, <a href="/search/physics?searchtype=author&query=Delahaye%2C+F">F. Delahaye</a>, <a href="/search/physics?searchtype=author&query=Zeippen%2C+C+J">C. J. Zeippen</a>, <a href="/search/physics?searchtype=author&query=Bastiani-Ceccotti%2C+S">S. Bastiani-Ceccotti</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="1201.6245v1-abstract-short" style="display: inline;"> Opacity is an important ingredient of the evolution of stars. The calculation of opacity coefficients is complicated by the fact that the plasma contains partially ionized heavy ions that contribute to opacity dominated by H and He. Up to now, the astrophysical community has greatly benefited from the work of the contributions of Los Alamos [1], Livermore [2] and the Opacity Project (OP) [3]. Howe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.6245v1-abstract-full').style.display = 'inline'; document.getElementById('1201.6245v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1201.6245v1-abstract-full" style="display: none;"> Opacity is an important ingredient of the evolution of stars. The calculation of opacity coefficients is complicated by the fact that the plasma contains partially ionized heavy ions that contribute to opacity dominated by H and He. Up to now, the astrophysical community has greatly benefited from the work of the contributions of Los Alamos [1], Livermore [2] and the Opacity Project (OP) [3]. However unexplained differences of up to 50% in the radiative forces and Rosseland mean values for Fe have been noticed for conditions corresponding to stellar envelopes. Such uncertainty has a real impact on the understanding of pulsating stellar envelopes, on the excitation of modes, and on the identification of the mode frequencies. Temperature and density conditions equivalent to those found in stars can now be produced in laboratory experiments for various atomic species. Recently the photo-absorption spectra of nickel and iron plasmas have been measured during the LULI 2010 campaign, for temperatures between 15 and 40 eV and densities of ~3 mg/cm3. A large theoretical collaboration, the "OPAC", has been formed to prepare these experiments. We present here the set of opacity calculations performed by eight different groups for conditions relevant to the LULI 2010 experiment and to astrophysical stellar envelope conditions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.6245v1-abstract-full').style.display = 'none'; document.getElementById('1201.6245v1-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> 30 January, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">15 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> High Energy Density Physics 7 (2011) 312-319 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1201.4692">arXiv:1201.4692</a> <span> [<a href="https://arxiv.org/pdf/1201.4692">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Atomic Physics">physics.atom-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-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/10.1051/epjconf/20135914003">10.1051/epjconf/20135914003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Iron and Nickel spectral opacity calculations in conditions relevant for pulsating stellar envelopes and experiments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Gilles%2C+D">D. Gilles</a>, <a href="/search/physics?searchtype=author&query=Turck-Chi%C3%A8ze%2C+S">S. Turck-Chi猫ze</a>, <a href="/search/physics?searchtype=author&query=Busquet%2C+M">M. Busquet</a>, <a href="/search/physics?searchtype=author&query=Thais%2C+F">F. Thais</a>, <a href="/search/physics?searchtype=author&query=Loisel%2C+G">G. Loisel</a>, <a href="/search/physics?searchtype=author&query=Piau%2C+L">L. Piau</a>, <a href="/search/physics?searchtype=author&query=Ducret%2C+J+E">J. E. Ducret</a>, <a href="/search/physics?searchtype=author&query=Blenski%2C+T">T. Blenski</a>, <a href="/search/physics?searchtype=author&query=Blancard%2C+C">C. Blancard</a>, <a href="/search/physics?searchtype=author&query=Coss%C3%A9%2C+P">P. Coss茅</a>, <a href="/search/physics?searchtype=author&query=Faussurier%2C+G">G. Faussurier</a>, <a href="/search/physics?searchtype=author&query=Gilleron%2C+F">F. Gilleron</a>, <a href="/search/physics?searchtype=author&query=Pain%2C+J+C">J. C. Pain</a>, <a href="/search/physics?searchtype=author&query=Porcherot%2C+Q">Q. Porcherot</a>, <a href="/search/physics?searchtype=author&query=Guzik%2C+J+A">J. A. Guzik</a>, <a href="/search/physics?searchtype=author&query=Kilcrease%2C+D+P">D. P. Kilcrease</a>, <a href="/search/physics?searchtype=author&query=Magee%2C+N+H">N. H. Magee</a>, <a href="/search/physics?searchtype=author&query=Harris%2C+J">J. Harris</a>, <a href="/search/physics?searchtype=author&query=Bastiani-Ceccotti%2C+S">S. Bastiani-Ceccotti</a>, <a href="/search/physics?searchtype=author&query=Delahaye%2C+F">F. Delahaye</a>, <a href="/search/physics?searchtype=author&query=Zeippen%2C+C+J">C. J. Zeippen</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="1201.4692v1-abstract-short" style="display: inline;"> Seismology of stars is strongly developing. To address this question we have formed an international collaboration OPAC to perform specific experimental measurements, compare opacity calculations and improve the opacity calculations in the stellar codes [1]. We consider the following opacity codes: SCO, CASSANDRA, STA, OPAS, LEDCOP, OP, SCO-RCG. Their comparison has shown large differences for Fe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.4692v1-abstract-full').style.display = 'inline'; document.getElementById('1201.4692v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1201.4692v1-abstract-full" style="display: none;"> Seismology of stars is strongly developing. To address this question we have formed an international collaboration OPAC to perform specific experimental measurements, compare opacity calculations and improve the opacity calculations in the stellar codes [1]. We consider the following opacity codes: SCO, CASSANDRA, STA, OPAS, LEDCOP, OP, SCO-RCG. Their comparison has shown large differences for Fe and Ni in equivalent conditions of envelopes of type II supernova precursors, temperatures between 15 and 40 eV and densities of a few mg/cm3 [2, 3, 4]. LEDCOP, OPAS, SCO-RCG structure codes and STA give similar results and differ from OP ones for the lower temperatures and for spectral interval values [3]. In this work we discuss the role of Configuration Interaction (CI) and the influence of the number of used configurations. We present and include in the opacity code comparisons new HULLAC-v9 calculations [5, 6] that include full CI. To illustrate the importance of this effect we compare different CI approximations (modes) available in HULLAC-v9 [7]. These results are compared to previous predictions and to experimental data. Differences with OP results are discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.4692v1-abstract-full').style.display = 'none'; document.getElementById('1201.4692v1-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> 23 January, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">4 pages, 3 figures, conference Inertial Fusion Sciences and Applications, Bordeaux, 12th to 16th September 2011; EPJ web of Conferences 2012</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1101.1170">arXiv:1101.1170</a> <span> [<a href="https://arxiv.org/pdf/1101.1170">pdf</a>, <a href="https://arxiv.org/format/1101.1170">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-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/10.1007/s10509-010-0583-8">10.1007/s10509-010-0583-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radiative properties of stellar plasmas and open challenges </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Turck-Chi%C3%A8ze%2C+S">S. Turck-Chi猫ze</a>, <a href="/search/physics?searchtype=author&query=Loisel%2C+G">G. Loisel</a>, <a href="/search/physics?searchtype=author&query=Gilles%2C+D">D. Gilles</a>, <a href="/search/physics?searchtype=author&query=Piau%2C+L">L. Piau</a>, <a href="/search/physics?searchtype=author&query=Blancard%2C+C">C. Blancard</a>, <a href="/search/physics?searchtype=author&query=Blenski%2C+T">T. Blenski</a>, <a href="/search/physics?searchtype=author&query=Busquet%2C+M">M. Busquet</a>, <a href="/search/physics?searchtype=author&query=Caillaud%2C+T">T. Caillaud</a>, <a href="/search/physics?searchtype=author&query=Coss%C3%A9%2C+P">P. Coss茅</a>, <a href="/search/physics?searchtype=author&query=Delahaye%2C+F">F. Delahaye</a>, <a href="/search/physics?searchtype=author&query=Faussurier%2C+G">G. Faussurier</a>, <a href="/search/physics?searchtype=author&query=Fariaut%2C+J">J. Fariaut</a>, <a href="/search/physics?searchtype=author&query=Gilleron%2C+F">F. Gilleron</a>, <a href="/search/physics?searchtype=author&query=Guzik%2C+J+A">J. A. Guzik</a>, <a href="/search/physics?searchtype=author&query=Harris%2C+J">J. Harris</a>, <a href="/search/physics?searchtype=author&query=Kilcrease%2C+D+P">D. P. Kilcrease</a>, <a href="/search/physics?searchtype=author&query=Magee%2C+N+H">N. H. Magee</a>, <a href="/search/physics?searchtype=author&query=Pain%2C+J+C">J. C. Pain</a>, <a href="/search/physics?searchtype=author&query=Porcherot%2C+Q">Q. Porcherot</a>, <a href="/search/physics?searchtype=author&query=Poirier%2C+M">M. Poirier</a>, <a href="/search/physics?searchtype=author&query=Soullier%2C+G">G. Soullier</a>, <a href="/search/physics?searchtype=author&query=Zeippen%2C+C+J">C. J. Zeippen</a>, <a href="/search/physics?searchtype=author&query=Bastiani-Ceccotti%2C+S">S. Bastiani-Ceccotti</a>, <a href="/search/physics?searchtype=author&query=Reverdin%2C+C">C. Reverdin</a>, <a href="/search/physics?searchtype=author&query=Silvert%2C+V">V. Silvert</a> , et al. (2 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="1101.1170v1-abstract-short" style="display: inline;"> The lifetime of solar-like stars, the envelope structure of more massive stars, and stellar acoustic frequencies largely depend on the radiative properties of the stellar plasma. Up to now, these complex quantities have been estimated only theoretically. The development of the powerful tools of helio- and astero- seismology has made it possible to gain insights on the interiors of stars. Consequen… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1101.1170v1-abstract-full').style.display = 'inline'; document.getElementById('1101.1170v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1101.1170v1-abstract-full" style="display: none;"> The lifetime of solar-like stars, the envelope structure of more massive stars, and stellar acoustic frequencies largely depend on the radiative properties of the stellar plasma. Up to now, these complex quantities have been estimated only theoretically. The development of the powerful tools of helio- and astero- seismology has made it possible to gain insights on the interiors of stars. Consequently, increased emphasis is now placed on knowledge of the monochromatic opacity coefficients. Here we review how these radiative properties play a role, and where they are most important. We then concentrate specifically on the envelopes of $尾$ Cephei variable stars. We discuss the dispersion of eight different theoretical estimates of the monochromatic opacity spectrum and the challenges we need to face to check these calculations experimentally. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1101.1170v1-abstract-full').style.display = 'none'; document.getElementById('1101.1170v1-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> 6 January, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">6 pages, 5 figures, in press (conference HEDLA 2010)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys. Space Science 2011 </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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