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Automatic Framework for Designing of Resilient IoT Applications </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Pessoa%2C+L+E">Luis Eduardo Pessoa</a>, <a href="/search/?searchtype=author&query=Iglesias%2C+C+F">Cristovao Freitas Iglesias Jr</a>, <a href="/search/?searchtype=author&query=Miceli%2C+C">Claudio Miceli</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="2411.18324v1-abstract-short" style="display: inline;"> Designing resilient Internet of Things (IoT) systems requires i) identification of IoT Critical Objects (ICOs) such as services, devices, and resources, ii) threat analysis, and iii) mitigation strategy selection. However, the traditional process for designing resilient IoT systems is still manual, leading to inefficiencies and increased risks. In addition, while tools such as ChatGPT could suppor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.18324v1-abstract-full').style.display = 'inline'; document.getElementById('2411.18324v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.18324v1-abstract-full" style="display: none;"> Designing resilient Internet of Things (IoT) systems requires i) identification of IoT Critical Objects (ICOs) such as services, devices, and resources, ii) threat analysis, and iii) mitigation strategy selection. However, the traditional process for designing resilient IoT systems is still manual, leading to inefficiencies and increased risks. In addition, while tools such as ChatGPT could support this manual and highly error-prone process, their use raises concerns over data privacy, inconsistent outputs, and internet dependence. Therefore, we propose RITA, an automated, open-source framework that uses a fine-tuned RoBERTa-based Named Entity Recognition (NER) model to identify ICOs from IoT requirement documents, correlate threats, and recommend countermeasures. RITA operates entirely offline and can be deployed on-site, safeguarding sensitive information and delivering consistent outputs that enhance standardization. In our empirical evaluation, RITA outperformed ChatGPT in four of seven ICO categories, particularly in actuator, sensor, network resource, and service identification, using both human-annotated and ChatGPT-generated test data. These findings indicate that RITA can improve resilient IoT design by effectively supporting key security operations, offering a practical solution for developing robust IoT architectures. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.18324v1-abstract-full').style.display = 'none'; document.getElementById('2411.18324v1-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.11988">arXiv:2409.11988</a> <span> [<a href="https://arxiv.org/pdf/2409.11988">pdf</a>, <a href="https://arxiv.org/format/2409.11988">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> </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/10.1051/0004-6361/202348907">10.1051/0004-6361/202348907 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-ray view of emission lines in optical spectra: Spectral analysis of the two low-mass X-ray binary systems Swift J1357.2-0933 and MAXI J1305-704 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Anitra%2C+A">A. Anitra</a>, <a href="/search/?searchtype=author&query=Miceli%2C+C">C. Miceli</a>, <a href="/search/?searchtype=author&query=Di+Salvo%2C+T">T. Di Salvo</a>, <a href="/search/?searchtype=author&query=Iaria%2C+R">R. Iaria</a>, <a href="/search/?searchtype=author&query=Degenaar%2C+N">N. Degenaar</a>, <a href="/search/?searchtype=author&query=Miller%2C+M+J">M. Jon Miller</a>, <a href="/search/?searchtype=author&query=Barra%2C+F">F. Barra</a>, <a href="/search/?searchtype=author&query=Leone%2C+W">W. Leone</a>, <a href="/search/?searchtype=author&query=Burderi%2C+L">L. Burderi</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="2409.11988v1-abstract-short" style="display: inline;"> We propose a novel approach for determining the orbital inclination of low-mass X-ray binary systems by modelling the H$伪$ and H$尾$ line profiles emitted by the accretion disc, with a Newtonian version of diskline. We applied the model to two sample sources, Swift J1357.2-0933 and MAXI J1305-704, which are both transient black hole systems, and analyse two observations that were collected during a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.11988v1-abstract-full').style.display = 'inline'; document.getElementById('2409.11988v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.11988v1-abstract-full" style="display: none;"> We propose a novel approach for determining the orbital inclination of low-mass X-ray binary systems by modelling the H$伪$ and H$尾$ line profiles emitted by the accretion disc, with a Newtonian version of diskline. We applied the model to two sample sources, Swift J1357.2-0933 and MAXI J1305-704, which are both transient black hole systems, and analyse two observations that were collected during a quiescent state and one observation of an outburst. The line profile is well described by the diskline model, although we had to add a Gaussian line to describe the deep inner core of the double-peaked profile, which the diskline model was unable to reproduce. The H$尾$ emission lines in the spectrum of Swift J1357.2-0933 and the H$伪$ emission lines in that of MAXI J1305-704 during the quiescent state are consistent with a scenario in which these lines originate from a disc ring between $(9.6-57) \times 10^{3}, \rm{R_{g}}$ and $(1.94-20) \times 10^{4}, \rm{R_{g}}$, respectively. We estimate an inclination angle of $81 \pm 5$ degrees for Swift J1357.2-0933 and an angle of $73 \pm 4$ degrees for MAXI J1305-704. This is entirely consistent with the values reported in the literature. In agreement with the recent literature, our analysis of the outburst spectrum of MAXI J1305-704 revealed that the radius of the emission region deviates from expected values. This outcome implies several potential scenarios, including alternative disc configuration or even a circumbinary disc. We caution that these results were derived from a simplistic model that may not fully describe the complicated physics of accretion discs. Despite these limitations, our results for the inclination angles are remarkably consistent with recent complementary studies, and the proposed description of the emitting region remains entirely plausible. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.11988v1-abstract-full').style.display = 'none'; document.getElementById('2409.11988v1-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> 18 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </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">11 pages, 7 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/2408.06856">arXiv:2408.06856</a> <span> [<a href="https://arxiv.org/pdf/2408.06856">pdf</a>, <a href="https://arxiv.org/format/2408.06856">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> </div> </div> <p class="title is-5 mathjax"> X-ray and optical polarization aligned with the radio jet ejecta in GX 339-4 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mastroserio%2C+G">G. Mastroserio</a>, <a href="/search/?searchtype=author&query=De+Marco%2C+B">B. De Marco</a>, <a href="/search/?searchtype=author&query=Baglio%2C+M+C">M. C. Baglio</a>, <a href="/search/?searchtype=author&query=Carotenuto%2C+F">F. Carotenuto</a>, <a href="/search/?searchtype=author&query=Fabiani%2C+S">S. Fabiani</a>, <a href="/search/?searchtype=author&query=Russell%2C+T+D">T. D. Russell</a>, <a href="/search/?searchtype=author&query=Capitanio%2C+F">F. Capitanio</a>, <a href="/search/?searchtype=author&query=Cavecchi%2C+Y">Y. Cavecchi</a>, <a href="/search/?searchtype=author&query=Motta%2C+S">S. Motta</a>, <a href="/search/?searchtype=author&query=Russell%2C+D+M">D. M. Russell</a>, <a href="/search/?searchtype=author&query=Dovciak%2C+M">M. Dovciak</a>, <a href="/search/?searchtype=author&query=Del+Santo%2C+M">M. Del Santo</a>, <a href="/search/?searchtype=author&query=Alabarta%2C+K">K. Alabarta</a>, <a href="/search/?searchtype=author&query=Ambrifi%2C+A">A. Ambrifi</a>, <a href="/search/?searchtype=author&query=Campana%2C+S">S. Campana</a>, <a href="/search/?searchtype=author&query=Casella%2C+P">P. Casella</a>, <a href="/search/?searchtype=author&query=Covino%2C+S">S. Covino</a>, <a href="/search/?searchtype=author&query=Illiano%2C+G">G. Illiano</a>, <a href="/search/?searchtype=author&query=Kara%2C+E">E. Kara</a>, <a href="/search/?searchtype=author&query=Lai%2C+E+V">E. V. Lai</a>, <a href="/search/?searchtype=author&query=Lodato%2C+G">G. Lodato</a>, <a href="/search/?searchtype=author&query=Manca%2C+A">A. Manca</a>, <a href="/search/?searchtype=author&query=Mariani%2C+I">I. Mariani</a>, <a href="/search/?searchtype=author&query=Marino%2C+A">A. Marino</a>, <a href="/search/?searchtype=author&query=Miceli%2C+C">C. Miceli</a> , et al. (5 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="2408.06856v1-abstract-short" style="display: inline;"> We present the first X-ray polarization measurements of GX 339-4. IXPE observed this source twice during its 2023-2024 outburst, once in the soft-intermediate state and again during a soft state. The observation taken during the intermediate state shows significant ($4蟽$) polarization degree P = $1.3\% \pm 0.3\%$ and polarization angle $胃$ = -74\degree $\pm$ 7\degree only in the 3 - 8 keV band. FO… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.06856v1-abstract-full').style.display = 'inline'; document.getElementById('2408.06856v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.06856v1-abstract-full" style="display: none;"> We present the first X-ray polarization measurements of GX 339-4. IXPE observed this source twice during its 2023-2024 outburst, once in the soft-intermediate state and again during a soft state. The observation taken during the intermediate state shows significant ($4蟽$) polarization degree P = $1.3\% \pm 0.3\%$ and polarization angle $胃$ = -74\degree $\pm$ 7\degree only in the 3 - 8 keV band. FORS2 at VLT observed the source simultaneously detecting optical polarization in the B, V, R, I bands (between $0.1%$ and $0.7\%$), all roughly aligned with the X-ray polarization. We also detect a discrete jet knot from radio observations taken later in time; this knot would have been ejected from the system around the same time as the hard-to-soft X-ray state transition and a bright radio flare occurred $\sim$3 months earlier. The proper motion of the jet knot provides a direct measurement of the jet orientation angle on the plane of the sky at the time of the ejection. We find that both the X-ray and optical polarization angles are aligned with the direction of the ballistic jet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.06856v1-abstract-full').style.display = 'none'; document.getElementById('2408.06856v1-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </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">Submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.11203">arXiv:2404.11203</a> <span> [<a href="https://arxiv.org/pdf/2404.11203">pdf</a>, <a href="https://arxiv.org/format/2404.11203">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> </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/10.1051/0004-6361/202449299">10.1051/0004-6361/202449299 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The puzzling orbital residuals of XTE J1710-281: is a Jovian planet orbiting around the binary system? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Iaria%2C+R">R. Iaria</a>, <a href="/search/?searchtype=author&query=Di+Salvo%2C+T">T. Di Salvo</a>, <a href="/search/?searchtype=author&query=Anitra%2C+A">A. Anitra</a>, <a href="/search/?searchtype=author&query=Miceli%2C+C">C. Miceli</a>, <a href="/search/?searchtype=author&query=Leone%2C+W">W. Leone</a>, <a href="/search/?searchtype=author&query=Maraventano%2C+C">C. Maraventano</a>, <a href="/search/?searchtype=author&query=Barra%2C+F">F. Barra</a>, <a href="/search/?searchtype=author&query=Riggio%2C+A">A. Riggio</a>, <a href="/search/?searchtype=author&query=Sanna%2C+A">A. Sanna</a>, <a href="/search/?searchtype=author&query=Manca%2C+A">A. Manca</a>, <a href="/search/?searchtype=author&query=Burderi%2C+L">L. Burderi</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="2404.11203v1-abstract-short" style="display: inline;"> XTE J1710-281 is a transient eclipsing binary system with a period close to 3.28 hours, hosting a neutron star. The average eclipse duration is 420 seconds, and eclipse arrival times reported in the literature span from 1999 to 2017. A previous analysis of the eclipse arrival times using the eclipse timing technique revealed a complex pattern of delays, indicating the presence of three orbital gli… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.11203v1-abstract-full').style.display = 'inline'; document.getElementById('2404.11203v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.11203v1-abstract-full" style="display: none;"> XTE J1710-281 is a transient eclipsing binary system with a period close to 3.28 hours, hosting a neutron star. The average eclipse duration is 420 seconds, and eclipse arrival times reported in the literature span from 1999 to 2017. A previous analysis of the eclipse arrival times using the eclipse timing technique revealed a complex pattern of delays, indicating the presence of three orbital glitches. These glitches correspond to sudden variations in the orbital period, allowing for the identification of four distinct epochs. We have re-analyzed the 78 eclipse arrival times spanning 18 years utilizing the eclipse timing technique to derive the corresponding delays as a function of time. We find that the observed delays align well with a fitting model employing an eccentric sine function characterized by an amplitude of $6.1 \pm 0.5$ s, eccentricity of $0.38 \pm 0.17$, and a period of $17.1 \pm 1.5$ years. Additionally, we identified the orbital period as 3.28106345(13) hours, with a reference epoch of $T_0=54112.83200(2)$ Modified Julian Date (MJD). We obtained an upper limit of the orbital period derivative of $3.6 \times 10^{-13}$ s~s$^{-1}$. From the average value of the eclipse duration, we estimate that the companion star has a mass of 0.22~\Msun for a neutron star mass of 1.4~\Msun, and the inclination of the source is $78.1^{+1.5}_{-1.2}$ degrees. The companion star is in thermal equilibrium. The orbital period derivative is consistent with a conservative mass transfer scenario, where the angular momentum loss due to magnetic braking dominates over gravitational radiation angular momentum loss if the former is present. The eccentric modulation can be explained by a third body with a mass of 2.7 Jovian masses, orbiting with a revolution period close to 17 years and an eccentricity of 0.38. (abridged abstract) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.11203v1-abstract-full').style.display = 'none'; document.getElementById('2404.11203v1-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> 17 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </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">7 pages, 10 figures, accepted for the publication by A&A on 12/04/2024</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A216 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.03698">arXiv:2401.03698</a> <span> [<a href="https://arxiv.org/pdf/2401.03698">pdf</a>, <a href="https://arxiv.org/format/2401.03698">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> </div> </div> <p class="title is-5 mathjax"> Confirmation of the presence of a CRSF in the NICER spectrum of X 1822-371 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Iaria%2C+R">R. Iaria</a>, <a href="/search/?searchtype=author&query=Di+Salvo%2C+T">T. Di Salvo</a>, <a href="/search/?searchtype=author&query=Anitra%2C+A">A. Anitra</a>, <a href="/search/?searchtype=author&query=Miceli%2C+C">C. Miceli</a>, <a href="/search/?searchtype=author&query=Barra%2C+F">F. Barra</a>, <a href="/search/?searchtype=author&query=Leone%2C+W">W. Leone</a>, <a href="/search/?searchtype=author&query=Burderi%2C+L">L. Burderi</a>, <a href="/search/?searchtype=author&query=Sanna%2C+A">A. Sanna</a>, <a href="/search/?searchtype=author&query=Riggio%2C+A">A. Riggio</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="2401.03698v1-abstract-short" style="display: inline;"> X 1822-371 is an eclipsing binary system with a period close to 5.57 hr and an orbital period derivative $\dot{P}_{\rm orb}$ of 1.42(3)$\times 10^{-10}$ s s$^{-1}$. The extremely high value of its $\dot{P}_{\rm orb}$ is compatible with a super-Eddington mass transfer rate from the companion star and, consequently, an intrinsic luminosity at the Eddington limit. The source is also an X-ray pulsar,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.03698v1-abstract-full').style.display = 'inline'; document.getElementById('2401.03698v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.03698v1-abstract-full" style="display: none;"> X 1822-371 is an eclipsing binary system with a period close to 5.57 hr and an orbital period derivative $\dot{P}_{\rm orb}$ of 1.42(3)$\times 10^{-10}$ s s$^{-1}$. The extremely high value of its $\dot{P}_{\rm orb}$ is compatible with a super-Eddington mass transfer rate from the companion star and, consequently, an intrinsic luminosity at the Eddington limit. The source is also an X-ray pulsar, it shows a spin frequency of 1.69 Hz and is in a spin-up phase with a spin frequency derivative of $7.4 \times 10^{-12}$ Hz s$^{-1}$. Assuming a luminosity at the Eddington limit, a neutron star magnetic field strength of $B = 8 \times 10^{10}$ G is estimated. However, a direct measure of $B$ could be obtained observing a CRSF in the energy spectrum. Analysis of \textit{XMM-Newton} data suggested the presence of a cyclotron line at 0.73 keV, with an estimated magnetic field strength of $B=(8.8 \pm 0.3) \times 10^{10}$ G. Here we analyze the 0.3-50 keV broadband spectrum of X 1822-371 combining a 0.3-10 keV NICER spectrum and a 4.5-50 keV \textit{NuSTAR} spectrum to investigate the presence of a cyclotron absorption line and the complex continuum emission spectrum. The NICER spectrum confirms the presence of a cyclotron line at 0.66 keV. The continuum emission is modeled with a Comptonized component, a thermal component associated with the presence of an accretion disk truncated at the magnetospheric radius of 105 km and a reflection component from the disk blurred by relativistic effects. We confirm the presence of a cyclotron line at 0.66 keV inferring a NS magnetic field of $B = (7.9\pm 0.5) \times 10^{10}$ G and suggesting that the Comptonized component originates in the accretion columns. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.03698v1-abstract-full').style.display = 'none'; document.getElementById('2401.03698v1-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> 8 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </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">16 pages, 16 figures, Accepte for publication in A&A on December 28, 2023</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.12636">arXiv:2310.12636</a> <span> [<a href="https://arxiv.org/pdf/2310.12636">pdf</a>, <a href="https://arxiv.org/ps/2310.12636">ps</a>, <a href="https://arxiv.org/format/2310.12636">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="High Energy Physics - Phenomenology">hep-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/10.1051/0004-6361/202346909">10.1051/0004-6361/202346909 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> H$尾$ spectroscopy of the high-inclination black hole transient Swift J1357.2-0933 during quiescence </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Anitra%2C+A">A. Anitra</a>, <a href="/search/?searchtype=author&query=Sanchez%2C+D+M">D. Mata Sanchez</a>, <a href="/search/?searchtype=author&query=Munoz-Darias%2C+T">T. Munoz-Darias</a>, <a href="/search/?searchtype=author&query=Di+Salvo%2C+T">T. Di Salvo</a>, <a href="/search/?searchtype=author&query=Iaria%2C+R">R. Iaria</a>, <a href="/search/?searchtype=author&query=Miceli%2C+C">C. Miceli</a>, <a href="/search/?searchtype=author&query=Padilla%2C+M+A">M. Armas Padilla</a>, <a href="/search/?searchtype=author&query=Casares%2C+J">J. Casares</a>, <a href="/search/?searchtype=author&query=Corral-Santana%2C+J+M">J. M. Corral-Santana</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="2310.12636v1-abstract-short" style="display: inline;"> Swift J1357.2-0933 is a transient low-mass X-ray binary hosting a stellar-mass black hole. The source exhibits optical dips and very broad emission lines during both outburst and quiescence, which are thought to be the result of a high orbital inclination. We present phase-resolved spectroscopy obtained with the 10.4m Gran Telescopio Canarias (GTC). The spectra focus on the $\rm{H}尾$ spectral regi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.12636v1-abstract-full').style.display = 'inline'; document.getElementById('2310.12636v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.12636v1-abstract-full" style="display: none;"> Swift J1357.2-0933 is a transient low-mass X-ray binary hosting a stellar-mass black hole. The source exhibits optical dips and very broad emission lines during both outburst and quiescence, which are thought to be the result of a high orbital inclination. We present phase-resolved spectroscopy obtained with the 10.4m Gran Telescopio Canarias (GTC). The spectra focus on the $\rm{H}尾$ spectral region during X-ray quiescence. The emission line is exceptionally broad (full width at half maximum, FWHM > 4000 脜), in agreement with previous studies focused on $\rm{H}伪$. A two-Gaussian fit to the prominent double-peaked profile reveals a periodic variability in the centroid position of the line. We also produced a diagnostic diagram aimed at constraining additional orbital parameters. Together, they allow us to independently confirm the orbital period of the system using a new dataset obtained five years after the previous outburst. However, our estimates for both the systemic velocity and the radial velocity semi-amplitude of the black hole reveal larger values than those found in previous studies. We argue that this could be explained by the precession of the disc and the presence of a hotspot. We found evidence of a narrow inner core in the double-peaked H$尾$ emission profile. We studied its evolution across the orbit, finding that it is likely to result from the occultation of inner material by the outer rim bulge, further supporting the high orbital inclination hypothesis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.12636v1-abstract-full').style.display = 'none'; document.getElementById('2310.12636v1-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> 19 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </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, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 679, A145 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.10429">arXiv:2306.10429</a> <span> [<a href="https://arxiv.org/pdf/2306.10429">pdf</a>, <a href="https://arxiv.org/format/2306.10429">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Software Engineering">cs.SE</span> </div> </div> <p class="title is-5 mathjax"> An Architectural Design Decision Model for Resilient IoT Application </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Iglesias%2C+C+F">Cristovao Freitas Iglesias Jr</a>, <a href="/search/?searchtype=author&query=Miceli%2C+C">Claudio Miceli</a>, <a href="/search/?searchtype=author&query=Bolic%2C+M">Miodrag Bolic</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="2306.10429v1-abstract-short" style="display: inline;"> The Internet of Things is a paradigm that refers to the ubiquitous presence around us of physical objects equipped with sensing, networking, and processing capabilities that allow them to cooperate with their environment to reach common goals. However, any threat affecting the availability of IoT applications can be crucial financially and for the safety of the physical integrity of users. This fe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.10429v1-abstract-full').style.display = 'inline'; document.getElementById('2306.10429v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.10429v1-abstract-full" style="display: none;"> The Internet of Things is a paradigm that refers to the ubiquitous presence around us of physical objects equipped with sensing, networking, and processing capabilities that allow them to cooperate with their environment to reach common goals. However, any threat affecting the availability of IoT applications can be crucial financially and for the safety of the physical integrity of users. This feature calls for IoT applications that remain operational and efficiently handle possible threats. However, designing an IoT application that can handle threats is challenging for stakeholders due to the high susceptibility to threats of IoT applications and the lack of modeling mechanisms that contemplate resilience as a first-class representation. In this paper, an architectural Design Decision Model for Resilient IoT applications is presented to reduce the difficulty of stakeholders in designing resilient IoT applications. Our approach is illustrated and demonstrates the value through the modeling of a case. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.10429v1-abstract-full').style.display = 'none'; document.getElementById('2306.10429v1-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> 17 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.00845">arXiv:2101.00845</a> <span> [<a href="https://arxiv.org/pdf/2101.00845">pdf</a>, <a href="https://arxiv.org/format/2101.00845">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cryptography and Security">cs.CR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Networking and Internet Architecture">cs.NI</span> </div> </div> <p class="title is-5 mathjax"> Crypto-Hotwire: Illegal Blockchain Mining at Zero Cost Using Public Infrastructures </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Coutinho%2C+F+R">Felipe Ribas Coutinho</a>, <a href="/search/?searchtype=author&query=Pires%2C+V">Victor Pires</a>, <a href="/search/?searchtype=author&query=Miceli%2C+C">Claudio Miceli</a>, <a href="/search/?searchtype=author&query=Menasche%2C+D+S">Daniel Sadoc Menasche</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="2101.00845v1-abstract-short" style="display: inline;"> Blockchains and cryptocurrencies disrupted the conversion of energy into a medium of exchange. Numerous applications for blockchains and cryptocurrencies are now envisioned for purposes ranging from inventory control to banking applications. Naturally, in order to mine in an economically viable way, regions where energy is plentiful and cheap, e.g., close to hydroelectric plants, are sought. The p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.00845v1-abstract-full').style.display = 'inline'; document.getElementById('2101.00845v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.00845v1-abstract-full" style="display: none;"> Blockchains and cryptocurrencies disrupted the conversion of energy into a medium of exchange. Numerous applications for blockchains and cryptocurrencies are now envisioned for purposes ranging from inventory control to banking applications. Naturally, in order to mine in an economically viable way, regions where energy is plentiful and cheap, e.g., close to hydroelectric plants, are sought. The possibility of converting energy into cash, however, also opens up opportunities for a new kind of cyber attack aimed at illegally mining cryptocurrencies by stealing energy. In this work, we indicate, using data from January and February of 2018 from our university, that such a threat is real, and present a projection of the gains derived from these attacks. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.00845v1-abstract-full').style.display = 'none'; document.getElementById('2101.00845v1-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> 4 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Symposium on Cryptocurrency Analysis (SOCCA) 2020 </p> </li> </ol> <div class="is-hidden-tablet"> <!-- feedback for mobile only --> <span class="help" style="display: inline-block;"><a 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