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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/2303.03392">arXiv:2303.03392</a> <span> [<a href="https://arxiv.org/pdf/2303.03392">pdf</a>, <a href="https://arxiv.org/format/2303.03392">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="Astrophysics of Galaxies">astro-ph.GA</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/acb775">10.3847/1538-4357/acb775 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Multiwavelength Classification and Study of Red Supergiant Candidates in NGC 6946 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+J+R">Jared R. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Koplitz%2C+B">Brad Koplitz</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+L">Leo Girardi</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="2303.03392v1-abstract-short" style="display: inline;"> We have combined resolved stellar photometry from Hubble Space Telescope (\emph{HST}), \emph{Spitzer}, and \emph{Gaia} to identify red supergiant (RSG) candidates in NGC~6946, based on their colors, proper motions, visual morphologies, and spectral energy distributions. We start with a large sample of 17,865 RSG candidates based solely on \emph{HST} near-infrared photometry. We then chose a small… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.03392v1-abstract-full').style.display = 'inline'; document.getElementById('2303.03392v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.03392v1-abstract-full" style="display: none;"> We have combined resolved stellar photometry from Hubble Space Telescope (\emph{HST}), \emph{Spitzer}, and \emph{Gaia} to identify red supergiant (RSG) candidates in NGC~6946, based on their colors, proper motions, visual morphologies, and spectral energy distributions. We start with a large sample of 17,865 RSG candidates based solely on \emph{HST} near-infrared photometry. We then chose a small sample of 385 of these candidates with Spitzer matches for more detailed study. Using evolutionary models and isochrones, we isolate a space where RSGs would be found in our photometry catalogs. We then visually inspect each candidate and compare to Gaia catalogs to identify and remove foreground stars. As a result, we classify 95 potential RSGs, with 40 of these being in our highest-quality sample. We fit the photometry of the populations of stars in the regions surrounding the RSGs to infer their ages. Placing our best candidate RSG stars into three age bins between 1 and 30 Myr, we find 27.5\% of the candidates falling between 1-10 Myr, 37.5\% between 10-20 Myr, and 35\% 20-30 Myr. A comparison of our results to the models of massive star evolution shows some agreement between model luminosities and the luminosities of our candidates for each age. Three of our candidates appear significantly more consistent with binary models than single-star evolution models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.03392v1-abstract-full').style.display = 'none'; document.getElementById('2303.03392v1-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">32 pages, 18 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.13621">arXiv:2107.13621</a> <span> [<a href="https://arxiv.org/pdf/2107.13621">pdf</a>, <a href="https://arxiv.org/ps/2107.13621">ps</a>, <a href="https://arxiv.org/format/2107.13621">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> </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/ac2a29">10.3847/1538-4357/ac2a29 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Solar Memory From Hours to Decades </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aschwanden%2C+M+J">Markus J. Aschwanden</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+J+R">Jay R. Johnson</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="2107.13621v1-abstract-short" style="display: inline;"> Waiting time distributions allow us to distinguish at least three different types of dynamical systems, such as (i) linear random processes (with no memory); (ii) nonlinear, avalanche-type, nonstationary Poisson processes (with memory during the exponential growth of the avalanche rise time); and (iii) chaotic systems in the state of a nonlinear limit cycle (with memory during the oscillatory phas… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.13621v1-abstract-full').style.display = 'inline'; document.getElementById('2107.13621v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.13621v1-abstract-full" style="display: none;"> Waiting time distributions allow us to distinguish at least three different types of dynamical systems, such as (i) linear random processes (with no memory); (ii) nonlinear, avalanche-type, nonstationary Poisson processes (with memory during the exponential growth of the avalanche rise time); and (iii) chaotic systems in the state of a nonlinear limit cycle (with memory during the oscillatory phase). We describe the temporal evolution of the flare rate $位(t) \propto t^p$ with a polynomial function, which allows us to distinguish linear ($p \approx 1$) from nonlinear ($p \gapprox 2$) events. The power law slopes $伪$ of observed waiting times (with full solar cycle coverage) cover a range of $伪=2.1-2.4$, which agrees well with our prediction of $伪= 2.0+1/p = 2.3-2.5$. The memory time can also be defined with the time evolution of the logistic equation, for which we find a relationship between the nonlinear growth time $蟿_G = 蟿_{rise}/(4p)$ and the nonlinearity index $p$. We find a nonlinear evolution for most events, in particular for the clustering of solar flares ($p=2.2\pm0.1$), partially occulted flare events ($p=1.8\pm0.2$), and the solar dynamo ($p=2.8\pm0.5$). The Sun exhibits memory on time scales of $\lapprox$2 hours to 3 days (for solar flare clustering), 6 to 23 days (for partially occulted flare events), and 1.5 month to 1 year (for the rise time of the solar dynamo). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.13621v1-abstract-full').style.display = 'none'; document.getElementById('2107.13621v1-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 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">11 pages, 1 Table, 5 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/2107.13065">arXiv:2107.13065</a> <span> [<a href="https://arxiv.org/pdf/2107.13065">pdf</a>, <a href="https://arxiv.org/ps/2107.13065">ps</a>, <a href="https://arxiv.org/format/2107.13065">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> </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/ac19a9">10.3847/1538-4357/ac19a9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Poissonian Origin of Power Laws in Solar Flare Waiting Time Distributions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aschwanden%2C+M+J">Markus J. Aschwanden</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+J+R">Jay R. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Nurhan%2C+Y+I">Yosia I. Nurhan</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="2107.13065v1-abstract-short" style="display: inline;"> In this study we aim for a deeper understanding of the power law slope, $伪$, of waiting time distributions. Statistically independent events with linear behavior can be characterized by binomial, Gaussian, exponential, or Poissonian size distribution functions. In contrast, physical processes with nonlinear behavior exhibit spatio-temporal coherence (or memory) and "fat tails" in their size distri… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.13065v1-abstract-full').style.display = 'inline'; document.getElementById('2107.13065v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.13065v1-abstract-full" style="display: none;"> In this study we aim for a deeper understanding of the power law slope, $伪$, of waiting time distributions. Statistically independent events with linear behavior can be characterized by binomial, Gaussian, exponential, or Poissonian size distribution functions. In contrast, physical processes with nonlinear behavior exhibit spatio-temporal coherence (or memory) and "fat tails" in their size distributions that fit power law-like functions, as a consequence of the time variability of the mean event rate, as demonstrated by means of Bayesian block decomposition in the work of Wheatland et al.~(1998). In this study we conduct numerical simulations of waiting time distributions $N(蟿)$ in a large parameter space for various (polynomial, sinusoidal, Gaussian) event rate functions $位(t)$, parameterized with an exponent $p$ that expresses the degree of the polynomial function $位(t) \propto t^p$. We derive an analytical exact solution of the waiting time distribution function in terms of the incomplete gamma function, which is similar to a Pareto type-II function and has a power law slope of $伪= 2 + 1/p$, in the asymptotic limit of large waiting times. Numerically simulated random distributions reproduce this theoretical prediction accurately. Numerical simulations in the nonlinear regime ($p \ge 2$) predict power law slopes in the range of $2.0 \le 伪\le 2.5$. The self-organized criticality model yields a prediction of $伪=2$. Observations of solar flares and coronal mass ejections (over at least a half solar cycle) are found in the range of $伪_{obs} \approx 2.1-2.4$. Deviations from strict power law functions are expected due to the variability of the flare event rate $位(t)$, and deviations from theoretically predicted slope values $伪$ occur due to the Poissonian weighting bias of power law fits. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.13065v1-abstract-full').style.display = 'none'; document.getElementById('2107.13065v1-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 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">14 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/2105.05939">arXiv:2105.05939</a> <span> [<a href="https://arxiv.org/pdf/2105.05939">pdf</a>, <a href="https://arxiv.org/format/2105.05939">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="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/10.1029/2021GL094348">10.1029/2021GL094348 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Role of the Solar Minimum in the Waiting Time Distribution Throughout the Heliosphere </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nurhan%2C+Y+I">Yosia I. Nurhan</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+J+R">Jay R. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Homan%2C+J+R">Jonathan R. Homan</a>, <a href="/search/astro-ph?searchtype=author&query=Wing%2C+S">Simon Wing</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="2105.05939v1-abstract-short" style="display: inline;"> We explore the tail of various waiting time datasets of processes that follow a nonstationary Poisson distribution with a sinusoidal driver. Analytically, we find that the distribution of large waiting times of such processes can be described using a power law slope of -2.5. We show that this result applies more broadly to any nonstationary Poisson process driven periodically. Examples of such pro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.05939v1-abstract-full').style.display = 'inline'; document.getElementById('2105.05939v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.05939v1-abstract-full" style="display: none;"> We explore the tail of various waiting time datasets of processes that follow a nonstationary Poisson distribution with a sinusoidal driver. Analytically, we find that the distribution of large waiting times of such processes can be described using a power law slope of -2.5. We show that this result applies more broadly to any nonstationary Poisson process driven periodically. Examples of such processes include solar flares, coronal mass ejections, geomagnetic storms, and substorms. We also discuss how the power law specifically relates to the behavior of driver near its minima. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.05939v1-abstract-full').style.display = 'none'; document.getElementById('2105.05939v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1710.08620">arXiv:1710.08620</a> <span> [<a href="https://arxiv.org/pdf/1710.08620">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</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.icarus.2017.10.043">10.1016/j.icarus.2017.10.043 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Retrieval of Water Vapor Column Abundance and Aerosol Properties from ChemCam Passive Sky Spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=McConnochie%2C+T+H">Timothy H. McConnochie</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M+D">Michael D. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Wolff%2C+M+J">Michael J. Wolff</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+S">Steve Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Lemmon%2C+M">Mark Lemmon</a>, <a href="/search/astro-ph?searchtype=author&query=Wiens%2C+R+C">Roger C. Wiens</a>, <a href="/search/astro-ph?searchtype=author&query=Maurice%2C+S">Sylvestre Maurice</a>, <a href="/search/astro-ph?searchtype=author&query=Gasnault%2C+O">Olivier Gasnault</a>, <a href="/search/astro-ph?searchtype=author&query=Lasue%2C+J">Jeremie Lasue</a>, <a href="/search/astro-ph?searchtype=author&query=Meslin%2C+P">Pierre-Yves Meslin</a>, <a href="/search/astro-ph?searchtype=author&query=Harri%2C+A">Ari-Matti Harri</a>, <a href="/search/astro-ph?searchtype=author&query=Genzer%2C+M">Maria Genzer</a>, <a href="/search/astro-ph?searchtype=author&query=Kemppinen%2C+O">Osku Kemppinen</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADnez%2C+G+M">Germ谩n M. Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=DeFlores%2C+L">Lauren DeFlores</a>, <a href="/search/astro-ph?searchtype=author&query=Blaney%2C+D">Diana Blaney</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+J+R">Jeffrey R. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+J+F">James F. Bell III</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="1710.08620v2-abstract-short" style="display: inline;"> We derive water vapor column abundances and aerosol properties from Mars Science Laboratory (MSL) ChemCam passive mode observations of scattered sky light. Each ChemCam passive sky observation acquires spectra at two different elevation angles. We fit these spectra with a discrete-ordinates multiple scattering radiative transfer model, using the correlated-k approximation for gas absorption band… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.08620v2-abstract-full').style.display = 'inline'; document.getElementById('1710.08620v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.08620v2-abstract-full" style="display: none;"> We derive water vapor column abundances and aerosol properties from Mars Science Laboratory (MSL) ChemCam passive mode observations of scattered sky light. Each ChemCam passive sky observation acquires spectra at two different elevation angles. We fit these spectra with a discrete-ordinates multiple scattering radiative transfer model, using the correlated-k approximation for gas absorption bands. The retrieval proceeds by first fitting the continuum of the ratio of the two elevation angles to solve for aerosol properties, and then fitting the continuum-removed ratio to solve for gas abundances. The final step of the retrieval makes use of the observed CO2 absorptions and the known CO2 abundance to correct the retrieved water vapor abundance for the effects of the vertical distribution of scattering aerosols and to derive an aerosol scale height parameter. The ChemCam-retrieved water abundances show, with only a few exceptions, the same seasonal behavior and the same timing of seasonal minima and maxima as the TES, CRISM, and REMS-H data sets that we compare them to. However ChemCam-retrieved water abundances are generally lower than zonal and regional scale from-orbit water vapor data, while at the same time being significantly larger than pre-dawn REMS-H abundances. Pending further analysis of REMS-H volume mixing ratio uncertainties, the differences between ChemCam and REMS-H pre-dawn mixing ratios appear to be much too large to be explained by large scale circulations and thus they tend to support the hypothesis of substantial diurnal interactions of water vapor with the surface. Our preliminary aerosol results, meanwhile, show the expected seasonal pattern in dust particle size but also indicate a surprising inter-annual increase in water-ice cloud opacities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.08620v2-abstract-full').style.display = 'none'; document.getElementById('1710.08620v2-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> 29 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2017. </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">64 pages with embedded figures; this is the accepted version of the manuscript; the meta-data version of the abstract has been shorted to meet arXiv rules</span> </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 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