A second planet transiting LTT 1445A and a determination of the masses of both worlds

K.H. acknowledges support from STFC grant ST/R000824/1.LTT 1445 is a hierarchical triple M-dwarf star system located at a distance of 6.86 pc. The primary star LTT 1445A (0.257 M⊙) is known to host the transiting planet LTT 1445Ab with an orbital period of 5.36 days, making it the second-closest known transiting exoplanet system, and the closest one for which the host is an M dwarf. Using Transiting Exoplanet Survey Satellite data, we present the discovery of a second planet in the LTT 1445 system, with an orbital period of 3.12 days. We combine radial-velocity measurements obtained from the five spectrographs, Echelle Spectrograph for Rocky Exoplanets and Stable Spectroscopic Observations, High Accuracy Radial Velocity Planet Searcher, High-Resolution Echelle Spectrometer, MAROON-X, and Planet Finder Spectrograph to establish that the new world also orbits LTT 1445A. We determine the mass and radius of LTT 1445Ab to be 2.87 ± 0.25 M⊕ and 1.304-0.060+0.067 R⊕, consistent with an Earth-like composition. For the newly discovered LTT 1445Ac, we measure a mass of 1.54-0.19+0.20 M⊕ and a minimum radius of 1.15 R⊕, but we cannot determine the radius directly as the signal-to-noise ratio of our light curve permits both grazing and nongrazing configurations. Using MEarth photometry and ground-based spectroscopy, we establish that star C (0.161 M⊙) is likely the source of the 1.4 day rotation period, and star B (0.215 M⊙) has a likely rotation period of 6.7 days. We estimate a probable rotation period of 85 days for LTT 1445A. Thus, this triple M-dwarf system appears to be in a special evolutionary stage where the most massive M dwarf has spun down, the intermediate mass M dwarf is in the process of spinning down, while the least massive stellar component has not yet begun to spin down.Publisher PDFPeer reviewe

Alliances to disseminate addiction prevention and treatment (ADAPT): A statewide learning health system to reduce substance use among justice-involved youth in rural communities.

BackgroundYouth in the justice system (YJS) are more likely than youth who have never been arrested to have mental health and substance use problems. However, a low percentage of YJS receive SUD services during their justice system involvement. The SUD care cascade can identify potential missed opportunities for treatment for YJS. Steps along the continuum of the cascade include identification of treatment need, referral to services, and treatment engagement. To address gaps in care for YJS, we will (1) implement a learning health system (LHS) to develop, or improve upon, alliances between juvenile justice (JJ) agencies and community mental health centers (CMHC) and (2) present local cascade data during continuous quality improvement cycles within the LHS alliances.Methods/designADAPT is a hybrid Type II effectiveness implementation trial. We will collaborate with JJ and CMHCs in eight Indiana counties. Application of the EPIS (exploration, preparation, implementation, and sustainment) framework will guide the implementation of the LHS alliances. The study team will review local cascade data quarterly with the alliances to identify gaps along the continuum. The study will collect self-report survey measures longitudinally at each site regarding readiness for change, implementation climate, organizational leadership, and program sustainability. The study will use the Stages of Implementation Completion (SIC) tool to assess the process of implementation across interventions. Additionally, the study team will conduct focus groups and qualitative interviews with JJ and CMHC personnel across the intervention period to assess for impact.DiscussionFindings have the potential to increase SUD need identification, referral to services, and treatment for YJS

A Second Planet Transiting LTT 1445A and a Determination of the Masses of Both Worlds

LTT 1445 is a hierarchical triple M-dwarf star system located at a distance of 6.86 pc. The primary star LTT 1445A (0.257 M ⊙) is known to host the transiting planet LTT 1445Ab with an orbital period of 5.36 days, making it the second-closest known transiting exoplanet system, and the closest one for which the host is an M dwarf. Using Transiting Exoplanet Survey Satellite data, we present the discovery of a second planet in the LTT 1445 system, with an orbital period of 3.12 days. We combine radial-velocity measurements obtained from the five spectrographs, Echelle Spectrograph for Rocky Exoplanets and Stable Spectroscopic Observations, High Accuracy Radial Velocity Planet Searcher, High-Resolution Echelle Spectrometer, MAROON-X, and Planet Finder Spectrograph to establish that the new world also orbits LTT 1445A. We determine the mass and radius of LTT 1445Ab to be 2.87 ± 0.25 M ⊕ and 1.304-0.060+0.067 R ⊕, consistent with an Earth-like composition. For the newly discovered LTT 1445Ac, we measure a mass of 1.54-0.19+0.20 M ⊕ and a minimum radius of 1.15 R ⊕, but we cannot determine the radius directly as the signal-to-noise ratio of our light curve permits both grazing and nongrazing configurations. Using MEarth photometry and ground-based spectroscopy, we establish that star C (0.161 M ⊙) is likely the source of the 1.4 day rotation period, and star B (0.215 M ⊙) has a likely rotation period of 6.7 days. We estimate a probable rotation period of 85 days for LTT 1445A. Thus, this triple M-dwarf system appears to be in a special evolutionary stage where the most massive M dwarf has spun down, the intermediate mass M dwarf is in the process of spinning down, while the least massive stellar component has not yet begun to spin down.Fil: Winters, Jennifer G.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Cloutier, Ryan. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Medina, Amber A.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Irwin, Jonathan M.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Charbonneau, David. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Astudillo Defru, Nicola. Universidad Católica de la Santísima Concepción; ChileFil: Bonfils, Xavier. Universite Grenoble Alpes; FranciaFil: Howard, Andrew W.. California Institute of Technology; Estados UnidosFil: Isaacson, Howard. University of California at Berkeley; Estados Unidos. The University of Queensland; AustraliaFil: Bean, Jacob L.. University of Chicago; Estados UnidosFil: Seifahrt, Andreas. University of Chicago; Estados UnidosFil: Teske, Johanna K.. University of Carnegie Mellon; Estados UnidosFil: Eastman, Jason D.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Twicken, Joseph D.. National Aeronautics and Space Administration; Estados UnidosFil: Collins, Karen A.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Jensen, Eric L. N.. Swarthmore College; Estados UnidosFil: Quinn, Samuel N.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Payne, Matthew J.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Kristiansen, Martti H.. Brorfelde Observatory; Dinamarca. Technical University of Denmark; DinamarcaFil: Spencer, Alton. Western Connecticut State University; Estados UnidosFil: Vanderburg, Andrew. Mit Kavli Institute For Astrophysics And Space Research; Estados UnidosFil: Zechmeister, Mathias. Universität Göttingen; AlemaniaFil: Weiss, Lauren M.. University of Notre Dame; Estados UnidosFil: Wang, Sharon Xuesong. Tsinghua University; ChinaFil: Diaz, Rodrigo Fernando. Vanderbilt University; Estados Unidos. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Brady, Madison. University of Chicago; Estados UnidosFil: Behmard, Aida. California Institute of Technology; Estados UnidosFil: Beard, Corey. University of California at Irvine; Estados UnidosFil: Batalha, Natalie M.. University of California; Estados UnidosFil: Almenara, Jose Manuel. Universite Grenoble Alpes; Francia. Centre National de la Recherche Scientifique; Franci

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Article discussing K-shell ionization elements Ca to Zn for 0.5 to 2.5-MeV/amu 14N-ion bombardment