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Featured submissions

September 2020

August 2020

July 2020

  • The UA Campus Repository team is thrilled about the launch of our sister repository, ReDATA. To deposit research datasets and code, please use the newly created UA Research Data Repository (ReDATA). ReDATA will curate the data and provide a DOI upon publication. Access is currently by request only. To obtain access, please contact data-management@arizona.edu.
  • Mass–Metallicity Trends in Transiting Exoplanets from Atmospheric Abundances of H2O, Na, and K

    Welbanks, Luis; Madhusudhan, Nikku; Allard, Nicole F.; Hubeny, Ivan; Spiegelman, Fernand; Leininger, Thierry; Univ Arizona, Dept Astron (IOP PUBLISHING LTD, 2019-12-11)
    Atmospheric compositions can provide powerful diagnostics of formation and migration histories of planetary systems. We investigate constraints on atmospheric abundances of H2O, Na, and K, in a sample of transiting exoplanets using the latest transmission spectra and new H-2 broadened opacities of Na and K. Our sample of 19 exoplanets spans from cool mini-Neptunes to hot Jupiters, with equilibrium temperatures between similar to 300 and 2700 K. Using homogeneous Bayesian retrievals we report atmospheric abundances of Na, K, and H2O, and their detection significances, confirming 6 planets with strong Na detections, 6 with K, and 14 with H2O. We find a mass-metallicity trend of increasing H2O abundances with decreasing mass, spanning generally substellar values for gas giants and stellar/superstellar for Neptunes and mini-Neptunes. However, the overall trend in H2O abundances, from mini-Neptunes to hot Jupiters, is significantly lower than the mass-metallicity relation for carbon in the solar system giant planets and similar predictions for exoplanets. On the other hand, the Na and K abundances for the gas giants are stellar or superstellar, consistent with each other, and generally consistent with the solar system metallicity trend. The H2O abundances in hot gas giants are likely due to low oxygen abundances relative to other elements rather than low overall metallicities, and provide new constraints on their formation mechanisms. The differing trends in the abundances of species argue against the use of chemical equilibrium models with metallicity as one free parameter in atmospheric retrievals, as different elements can be differently enhanced.
  • Drill core data for the Courtland-Gleeson area, Turquoise mining district and southern Dragoon Mountains, Cochise County, Arizona

    Richardson, C.A.; Arizona Geological Survey (Arizona Geological Survey (Tucson, AZ), 2020)
  • Constraining the Neutron Star Mass–Radius Relation and Dense Matter Equation of State with NICER. I. The Millisecond Pulsar X-Ray Data Set

    Bogdanov, Slavko; Guillot, Sebastien; Ray, Paul S.; Wolff, Michael T.; Chakrabarty, Deepto; Ho, Wynn C. G.; Kerr, Matthew; Lamb, Frederick K.; Lommen, Andrea; Ludlam, Renee M.; et al. (IOP PUBLISHING LTD, 2019-12-12)
    Atmospheric compositions can provide powerful diagnostics of formation and migration histories of planetary systems. We investigate constraints on atmospheric abundances of H2O, Na, and K, in a sample of transiting exoplanets using the latest transmission spectra and new H-2 broadened opacities of Na and K. Our sample of 19 exoplanets spans from cool mini-Neptunes to hot Jupiters, with equilibrium temperatures between similar to 300 and 2700 K. Using homogeneous Bayesian retrievals we report atmospheric abundances of Na, K, and H2O, and their detection significances, confirming 6 planets with strong Na detections, 6 with K, and 14 with H2O. We find a mass-metallicity trend of increasing H2O abundances with decreasing mass, spanning generally substellar values for gas giants and stellar/superstellar for Neptunes and mini-Neptunes. However, the overall trend in H2O abundances, from mini-Neptunes to hot Jupiters, is significantly lower than the mass-metallicity relation for carbon in the solar system giant planets and similar predictions for exoplanets. On the other hand, the Na and K abundances for the gas giants are stellar or superstellar, consistent with each other, and generally consistent with the solar system metallicity trend. The H2O abundances in hot gas giants are likely due to low oxygen abundances relative to other elements rather than low overall metallicities, and provide new constraints on their formation mechanisms. The differing trends in the abundances of species argue against the use of chemical equilibrium models with metallicity as one free parameter in atmospheric retrievals, as different elements can be differently enhanced.
  • The Acceleration and Confinement of Energetic Electrons by a Termination Shock in a Magnetic Trap: An Explanation for Nonthermal Loop-top Sources during Solar Flares

    Kong, Xiangliang; Guo, Fan; Shen, Chengcai; Chen, Bin; Chen, Yao; Musset, Sophie; Glesener, Lindsay; Pongkitiwanichakul, Peera; Giacalone, Joe; Univ Arizona, Dept Planetary Sci (IOP PUBLISHING LTD, 2019-12-20)
    We present the set of deep Neutron Star Interior Composition Explorer (NICER) X-ray timing observations of the nearby rotation-powered millisecond pulsars PSRs J0437-4715, J0030+0451, J1231-1411, and J2124-3358, selected as targets for constraining the mass-radius relation of neutron stars and the dense matter equation of state (EoS) via modeling of their pulsed thermal X-ray emission. We describe the instrument, observations, and data processing/reduction procedures, as well as the series of investigations conducted to ensure that the properties of the data sets are suitable for parameter estimation analyses to produce reliable constraints on the neutron star mass-radius relation and the dense matter EoS. We find that the long-term timing and flux behavior and the Fourier-domain properties of the event data do not exhibit any anomalies that could adversely affect the intended measurements. From phase-selected spectroscopy, we find that emission from the individual pulse peaks is well described by a single-temperature hydrogen atmosphere spectrum, with the exception of PSR J0437-4715, for which multiple temperatures are required.
  • Physical Characterization of the 2017 December Outburst of the Centaur 174P/Echeclus

    Kareta, Theodore; Sharkey, Benjamin; Noonan, John; Volk, Kat; Reddy, Vishnu; Harris, Walter; Miles, Richard; Univ Arizona, Lunar & Planetary Lab (IOP PUBLISHING LTD, 2019-12-04)
    The Centaurs are the small solar system bodies intermediate between the active inner solar system Jupiter family comets and their inactive progenitors in the trans-Neptunian region. Among the fraction of Centaurs which show comet-like activity, 174P/Echeclus is best known for its massive 2005 outburst in which a large apparently active fragment was ejected above the escape velocity from the primary nucleus. We present visible imaging and near-infrared spectroscopy of Echeclus during the first week after its 2017 December outburst taken at the Faulkes North and South Telescopes and the NASA IRTF, the largest outburst since 2005. The coma was seen to be highly asymmetric. A secondary peak was seen in the near-infrared 2D spectra, which is strongly hinted at in the visible images, moving hyperbolically with respect to the nucleus. The retrieved reflectance spectrum of Echelcus is consistent with the unobscured nucleus but becomes bluer when a wider extraction aperture is used. We find that Echeclus's coma is best explained as dominated by large blue dust grains, which agrees with previous work. We also conducted a high-resolution orbital integration of Echeclus's recent evolution and found no large orbital changes that could drive its modern evolution. We interpret the second peak in the visible and near-infrared data sets as a large cloud of larger-than-dust debris ejected at the time of outburst. If Echeclus is typical of the Centaurs, there may be several debris ejection or fragmentation events per year on other Centaurs that are going unnoticed.

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