Articoli Di Giuseppina Micela Su Riviste Con Referee (Ottobre 2019)

Total Page:16

File Type:pdf, Size:1020Kb

Articoli Di Giuseppina Micela Su Riviste Con Referee (Ottobre 2019) Articoli di Giuseppina Micela su riviste con referee (Ottobre 2019) Hojjatpanah S, Figueira P, Santos N C, Adibekyan V., Sousa S G, Delgado-Mena E, Alibert Y, Cristiani S, Gonzalez Hernandez J I, Lanza A F, Di Marcantonio P, Martins J H C, Micela G, Molaro P, Neves V, Oshagh M, Pepe F, Poretti E, Rojas-Ayala B, Rebolo R, Suarez Mascareno A, & Zapatero Osorio M R 2019, A&A, Catalog for the ESPRESSO blind radial velocity exoplanet survey https://ui.adsabs.harvard.edu/abs/2019A%26A...629A..80H Guarcello M G, Flaccomio E, Micela G, Argiroffi C, Sciortino S, Venuti L, Stauffer J, Rebull L. & Cody A M 2019, A&A, CSI 2264: Simultaneous optical and X-ray variability in the pre-main sequence stars of NGC 2264. II. Photometric variability, magnetic activity, and rotation in class III objects and stars with transition disKs https://ui.adsabs.harvard.edu/abs/2019A%26A...628A..74G Pizzocaro D, Stelzer B, Poretti E, Raetz S, Micela G, Belfiore A, Marelli M, Salvetti D, & De Luca A 2019, A&A, Activity and rotation of the X-ray emitting Kepler stars https://ui.adsabs.harvard.edu/abs/2019A%26A...628A..41P Collier Cameron A, Mortier A, Phillips D, Dumusque X, Haywood R D, Langellier N, Watson C A, Cegla H M, Costes J, Charbonneau D, Coffinet A, Latham D W, Lopez-Morales M, Malavolta L, Maldonado J, Micela G, Milbourne T, Molinari, E, Saar S H, Thompson S, Buchschacher N, Cecconi M, Cosentino R, Ghedina A, Glenday A, Gonzalez M, Li C-H, Lodi M, Lovis C, Pepe F, Poretti E, Rice K, Sasselov D, Sozzetti A, Szentgyorgyi A, Udry S, & Walsworth R 2019, MNRAS, Three years of Sun-as-a-star radial-velocity observations on the approach to solar minimum https://ui.adsabs.harvard.edu/abs/2019MNRAS.487.1082C Maldonado J, Phillips D, Dumusque X, Collier Cameron A, Haywood R D, Lanza A F, Micela G, Mortier A, Saar S, Sozzetti A, Rice K, Milbourne T, Cecconi M, Cegla H M, Cosentino R, Costes J, Ghedina A, Gonzalez M, Guerra J, Hernandez N, Li C-H, Lodi M, Malavolta L, Molinari E, Pepe F, Piotto G, Poretti E, Sasselov D, San Juan J, Thompson S, Udry S, & Watson C 2019, A&A, Temporal evolution and correlations of optical activity indicators measured in Sun-as-a-star observations https://ui.adsabs.harvard.edu/abs/2019A%26A...627A.118M Wright N J, Jeffries R, Jackson R., Bayo A, Bonito R, Damiani F, Kalari V, Lanzafame A, Pancino E, Parker R, Prisinzano L, Randich S, Vink J, Alfaro E, Bergemann M, Franciosini E, Gilmore G, Gonneau A, Hourihane A, Jofré P, Koposov S, Lewis J, Magrini L, Micela G, Morbidelli L, Sacco G, Worley C, & Zaggia S 2019, MNRAS, The Gaia- ESO Survey: asymmetric expansion of the Lagoon Nebula cluster NGC 6530 from GES and Gaia DR2 https://ui.adsabs.harvard.edu/abs/2019MNRAS.486.2477W Damiano M, Micela G, & Tinetti G. 2019, ApJ, Principal Component Analysis-based Method to Analyze High- resolution Spectroscopic Data on Exoplanets, https://ui.adsabs.harvard.edu/abs/2019ApJ...878..153D Guarcello M, Argiroffi C, Drake J, Flaccomio E, Lopez-Santiago J, Micela G, Reale F, Rebull L, Sciortino S, Stauffer J, Antoniou V, & Alvarado-Gomez J 2019, AN, Simultaneous Kepler/K2 and XMM-Newton observations of superflares in the Pleiades https://ui.adsabs.harvard.edu/abs/2019AN....340..302G Pinamonti M, Sozzetti A, Giacobbe P, Damasso M, Scandariato G, Perger M, Gonzalez Hernandez J, Lanza A, Maldonado J, Micela G, Suarez Mascareno A, Toledo-Padron B, Affer L, Benatti S, Bignamini A, Bonomo A, Claudi R, Cosentino R, Desidera S, Maggio A, Martinez Fiorenzano A, Pagano I, Piotto G, Rainer M, Rebolo R, & Ribas I 2019, A&A, The HADES RV programme with HARPS-N at TNG. XI. GJ 685 b: a warm super-Earth around an active M dwarf https://ui.adsabs.harvard.edu/abs/2019A%26A...625A.126P Rice K, Malavolta L, Mayo A, Mortier A, Buchhave L, Affer L, Vanderburg A, Lopez-Morales M, Poretti E, Zeng L, Collier Cameron A, Damasso M, Coffinet A, Latham D, Bonomo A S, Bouchy F, Charbonneau D, Dumusque X, Figueira P, Martinez Fiorenzano A, Haywood R, Johnson J, Lopez E, Lovis C, Mayor M, Micela G, Molinari E, Nascimbeni V, Nava C, Pepe F, Phillips D, Piotto G, Sasselov D, Segransan D, Sozzetti A, Udry S, & Watson C 2019, MNRAS, Masses and radii for the three super-Earths orbiting GJ 9827, and implications for the composition of small exoplanets https://ui.adsabs.harvard.edu/abs/2019MNRAS.484.3731R Borsato L, Malavolta L, Piotto G, Buchhave L, Mortier A, Rice K, Collier Cameron A, Coffinet A, Sozzetti A, Charbonneau D, Cosentino R, Dumusque X, Figueira P, Latham D, Lopez-Morales M, Mayor M, Micela G, Molinari E, Pepe F, Phillips D, Poretti E, Udry S, Watson C 2019, MNRAS, HARPS-N radial velocities confirm the low densities of the Kepler-9 planets https://ui.adsabs.harvard.edu/abs/2019MNRAS.484.3233B Perger M, Scandariato G, Ribas I, Morales J, Affer L, Azzaro M, Amado P, Anglada-Escudé G, Baroch D, Barrado D, Bauer F, Béjar V, Caballero J, Cortés-Contreras M, Damasso M, Dreizler S, Gonzalez-Cuesta L, Gonzalez Hernandez J, Guenther, E, Henning T, Herrero E, Jeffers S, Kaminski A, Kuerster M, Lafarga M, Leto G, Lopez-Gonzalez M, Maldonado J, Micela G, Montes D, Pinamonti M, Quirrenbach A, Rebolo R, Reiners A, Rodriguez E, Rodriguez- Lopez C, Schmitt J, Sozzetti A, Suarez Mascareno A, Toledo-Padron B, Zanmar Sanchez R, Zapatero Osorio M, & Zechmeister M 2019, A&A Gliese 49: activity evolution and detection of a super-Earth. A HADES and CARMENES Collaboration https://ui.adsabs.harvard.edu/abs/2019A%26A...624A.123P Locci D, Cecchi-Pestellini C, & Micela G 2019, A&A, Photo-evaporation of close-in gas giants orbiting around G and M stars https://ui.adsabs.harvard.edu/abs/2019A%26A...624A.101L Maldonado J, Villaver E, Eiroa C, & Micela G 2019, A&A Connecting substellar and stellar formation: the role of the host star's metallicity https://ui.adsabs.harvard.edu/abs/2019A%26A...624A..94M Gonzalez Alvarez E, Micela G, Maldonado J, Affer L, Maggio A, Lanza A F., Covino E, Benatti S, Bignamini A, Cosentino R, Damasso M, Desidera S, Gonzalez Hernandez J I., Martìnez-Fiorenzano A, Pagano I, Perger M, Piotto G, Pinamonti M, Rainer M, Rebolo R, Ribas I, Scandariato G, Sozzetti A, Suarez Mascareno A, & Toledo-Padron B 2019, A&A HADES RV Programme with HARPS-N at TNG. X. The non-saturated regime of the stellar activity- rotation relationship for M dwarfs https://ui.adsabs.harvard.edu/abs/2019A%26A...624A..27G Milbourne T W., Haywood R D., Phillips D F., Saar S H., Cegla H M., Cameron A C., Costes J, Dumusque X, Langellier N, Latham D W., Maldonado J, Malavolta L, Mortier A, Palumbo M L., III, Thompson S, Watson C A., Bouchy F, Buchschacher N, Cecconi M, Charbonneau D, Cosentino R, Ghedina A, Glenday A G., Gonzalez M, Li C-H., Lodi M, Lopez-Morales M, Lovis C, Mayor M, Micela G, Molinari E, Pepe F, Piotto G, Rice K, Sasselov D, Segransan D, Sozzetti A, Szentgyorgyi A, Udry S, & Walsworth R L. 2019, ApJ, HARPS-N Solar RVs Are Dominated by Large, Bright Magnetic Regions https://ui.adsabs.harvard.edu/abs/2019ApJ...874..107M Kosiarek M R, Blunt S, Lopez-Morales M, Crossfield I J M, Sinukoff E, Petigura E A, Gonzales E J, Poretti E, Malavolta L, Howard A W, Isaacson H, Haywood R D, Ciardi D R, Bristow M, Collier Cameron A, Charbonneau D, Dressing C D, Figueira P, Fulton B J, Hardee B J, Hirsch L A, Latham D W, Mortier A, Nava C, Schlieder J E, Vanderburg A, Weiss L, Bonomo A S, Bouchy F, Buchhave L A, Coffinet A, Damasso M, Dumusque X, Lovis C, Mayor M, Micela G, Molinari E, Pepe F, Phillips D, Piotto G, Rice K, Sasselov D, Segransan D, Sozzetti A, Udry S, & Watson C 2019, AJ, K2-291b: A RocKy Super-Earth in a 2.2 day Orbit https://ui.adsabs.harvard.edu/abs/2019AJ....157..116K Prisinzano L, Damiani F, Kalari V, Jeffries R, Bonito R, Micela G, Wright N J., Jackson R J., Tognelli E, Guarcello M, Vink J S., Klutsch A, Jimenez-Esteban F M., Roccatagliata V, Tautvaitiené; G, Gilmore G, Randich S, Alfaro E J., Flaccomio E, Koposov S, Lanzafame A, Pancino E, Bergemann M, Carraro G, Franciosini E, Frasca A, Gonneau A, Hourihane A, Jofré P., Lewis J, Magrini L, Monaco L, Morbidelli L, Sacco G G., Worley C C., & Zaggia S 2019, A&A The Gaia-ESO Survey: Age spread in the star forming region NGC 6530 from the HR diagram and gravity indicators https://ui.adsabs.harvard.edu/abs/2019A%26A...623A.159P Damiani F, Prisinzano L, Pillitteri I, Micela G, & Sciortino S 2019, A&A Stellar population of Sco OB2 revealed by Gaia DR2 data https://ui.adsabs.harvard.edu/abs/2019A%26A...623A.112D Pillitteri I, Sciortino S, Reale F, Micela G, Argiroffi C, Flaccomio E, &Stelzer B 2019, A&A Deep X-ray view of the Class I YSO Elias 29 with XMM-Newton and NuSTAR https://ui.adsabs.harvard.edu/abs/2019A%26A...623A..67P Damiani F, Prisinzano L, Micela G, & Sciortino S 2019, A&A, Wide-area photometric and astrometric (Gaia DR2) study of the young cluster NGC 6530 https://ui.adsabs.harvard.edu/abs/2019A%26A...623A..25D Bonomo A S, Zeng L, Damasso M, Leinhardt Z M, Justesen A B, Lopez E, Lund M N, Malavolta L, Silva A, V, Buchhave L A, Corsaro E, Denman T, Lopez-Morales M, Mills S M, Mortier A, Rice K, Sozzetti A, Vanderburg A, Affer L, Arentoft T, Benbakoura M, Bouchy F, Christensen-Dalsgaard J, Collier Cameron A, Cosentino R, Dressing C D, Dumusque X., Figueira P, Fiorenzano A F M, Garcia R A, Handberg R, Harutyunyan A, Johnson J A, Kjeldsen H, Latham D W, Lovis C, Lundkvist M S, Mathur S., Mayor M, Micela G, Molinari E, Motalebi F, Nascimbeni V, Nava C, Pepe F, Phillips D F, Piotto G, Poretti E, Sasselov D, Segransan D, Udry F, & Watson C 2019, Nature Astronomy A giant impact as the liKely origin of different twins in the Kepler-107 exoplanet
Recommended publications
  • Chemical Evolution of Protoplanetary Disks-The Effects of Viscous Accretion, Turbulent Mixing and Disk Winds
    Draft version June 5, 2018 Preprint typeset using LATEX style emulateapj v. 11/10/09 CHEMICAL EVOLUTION OF PROTOPLANETARY DISKS – THE EFFECTS OF VISCOUS ACCRETION, TURBULENT MIXING AND DISK WINDS D. Heinzeller1 and H. Nomura Department of Astronomy, Graduate School of Science, Kyoto University, Kyoto 606-8502, Japan and C. Walsh and T. J. Millar Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast, BT7 1NN, UK Draft version June 5, 2018 ABSTRACT We calculate the chemical evolution of protoplanetary disks considering radial viscous accretion, vertical turbulent mixing and vertical disk winds. We study the effects on the disk chemical structure when different models for the formation of molecular hydrogen on dust grains are adopted. Our gas- phase chemistry is extracted from the UMIST Database for Astrochemistry (Rate06) to which we have added detailed gas-grain interactions. We use our chemical model results to generate synthetic near- and mid-infrared LTE line emission spectra and compare these with recent Spitzer observations. Our results show that if H2 formation on warm grains is taken into consideration, the H2O and OH abundances in the disk surface increase significantly. We find the radial accretion flow strongly influences the molecular abundances, with those in the cold midplane layers particularly affected. On the other hand, we show that diffusive turbulent mixing affects the disk chemistry in the warm molecular layers, influencing the line emission from the disk and subsequently improving agreement with observations. We find that NH3, CH3OH, C2H2 and sulphur-containing species are greatly enhanced by the inclusion of turbulent mixing.
    [Show full text]
  • Lurking in the Shadows: Wide-Separation Gas Giants As Tracers of Planet Formation
    Lurking in the Shadows: Wide-Separation Gas Giants as Tracers of Planet Formation Thesis by Marta Levesque Bryan In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy CALIFORNIA INSTITUTE OF TECHNOLOGY Pasadena, California 2018 Defended May 1, 2018 ii © 2018 Marta Levesque Bryan ORCID: [0000-0002-6076-5967] All rights reserved iii ACKNOWLEDGEMENTS First and foremost I would like to thank Heather Knutson, who I had the great privilege of working with as my thesis advisor. Her encouragement, guidance, and perspective helped me navigate many a challenging problem, and my conversations with her were a consistent source of positivity and learning throughout my time at Caltech. I leave graduate school a better scientist and person for having her as a role model. Heather fostered a wonderfully positive and supportive environment for her students, giving us the space to explore and grow - I could not have asked for a better advisor or research experience. I would also like to thank Konstantin Batygin for enthusiastic and illuminating discussions that always left me more excited to explore the result at hand. Thank you as well to Dimitri Mawet for providing both expertise and contagious optimism for some of my latest direct imaging endeavors. Thank you to the rest of my thesis committee, namely Geoff Blake, Evan Kirby, and Chuck Steidel for their support, helpful conversations, and insightful questions. I am grateful to have had the opportunity to collaborate with Brendan Bowler. His talk at Caltech my second year of graduate school introduced me to an unexpected population of massive wide-separation planetary-mass companions, and lead to a long-running collaboration from which several of my thesis projects were born.
    [Show full text]
  • Physical Parameters of the Multiplanet Systems HD 106315 and GJ 9827*†
    The Astronomical Journal, 161:47 (16pp), 2021 January https://doi.org/10.3847/1538-3881/abca39 © 2020. The American Astronomical Society. All rights reserved. Physical Parameters of the Multiplanet Systems HD 106315 and GJ 9827*† Molly R. Kosiarek1,35 , David A. Berardo2 , Ian J. M. Crossfield3, Cesar Laguna1,4 , Caroline Piaulet5 , Joseph M. Akana Murphy1,35 , Steve B. Howell6 , Gregory W. Henry7 , Howard Isaacson8,9 , Benjamin Fulton10 , Lauren M. Weiss11 , Erik A. Petigura12 , Aida Behmard13 , Lea A. Hirsch14 , Johanna Teske15, Jennifer A. Burt16 , Sean M. Mills17 , Ashley Chontos18,35 , Teo Močnik19 , Andrew W. Howard17 , Michael Werner16 , John H. Livingston20 , Jessica Krick21 , Charles Beichman22 , Varoujan Gorjian16 , Laura Kreidberg23,24 , Caroline Morley25 , Jessie L. Christiansen21 , Farisa Y. Morales16 , Nicholas J. Scott6 , Jeffrey D. Crane26 , Sharon Xuesong Wang27,28 , Stephen A. Shectman26, Lee J. Rosenthal17 , Samuel K. Grunblatt29,30 , Ryan A. Rubenzahl17,35 , Paul A. Dalba31,36 , Steven Giacalone32 , Chiara Dane Villanueva1,4, Qingtian Liu1,4, Fei Dai13 , Michelle L. Hill31 , Malena Rice33 , Stephen R. Kane31 , and Andrew W. Mayo32,34 1 Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA; [email protected] 2 Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 3 Department of Physics & Astronomy, University of Kansas, 1082 Malott,1251 Wescoe Hall Dr., Lawrence, KS 66045, USA 4 Department
    [Show full text]
  • Naming the Extrasolar Planets
    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
    [Show full text]
  • Optical Spectroscopic Monitoring Observations of a T Tauri Star V409 Tau
    International Journal of Astronomy and Astrophysics, 2019, 9, 321-334 http://www.scirp.org/journal/ijaa ISSN Online: 2161-4725 ISSN Print: 2161-4717 Optical Spectroscopic Monitoring Observations of a T Tauri Star V409 Tau Hinako Akimoto, Yoichi Itoh Nishi-Harima Astronomical Observatory, Center for Astronomy, University of Hyogo, Hyogo, Japan How to cite this paper: Akimoto, H. and Abstract Itoh, Y. (2019) Optical Spectroscopic Mon- itoring Observations of a T Tauri Star V409 We report the results of optical spectroscopic monitoring observations of a T Tau. International Journal of Astronomy Tauri star, V409 Tau. A previous photometric study indicated that this star and Astrophysics, 9, 321-334. experienced dimming events due to the obscuration of light from the central https://doi.org/10.4236/ijaa.2019.93023 star with a distorted circumstellar disk. We conducted medium-resolution (R Received: July 24, 2019 ~10,000) spectroscopic observations with 2-m Nayuta telescope at Ni- Accepted: September 16, 2019 shi-Harima Astronomical Observatory. Spectra were obtained in 18 nights Published: September 19, 2019 between November 2015 and March 2016. Several absorption lines such as Ca Copyright © 2019 by author(s) and I and Li, and the Hα emission line were confirmed in the spectra. The Ic-band Scientific Research Publishing Inc. magnitudes of V409 Tau changed by approximately 1 magnitude during the This work is licensed under the Creative observation epoch. The equivalent widths of the five absorption lines are Commons Attribution International License (CC BY 4.0). roughly constant despite changes in the Ic-band magnitudes. We conclude http://creativecommons.org/licenses/by/4.0/ that the light variation of the star is caused by the obscuration of light from Open Access the central star with a distorted circumstellar disk, based on the relationship between the equivalent widths of the absorption lines and the Ic-band magni- tudes.
    [Show full text]
  • Exep Science Plan Appendix (SPA) (This Document)
    ExEP Science Plan, Rev A JPL D: 1735632 Release Date: February 15, 2019 Page 1 of 61 Created By: David A. Breda Date Program TDEM System Engineer Exoplanet Exploration Program NASA/Jet Propulsion Laboratory California Institute of Technology Dr. Nick Siegler Date Program Chief Technologist Exoplanet Exploration Program NASA/Jet Propulsion Laboratory California Institute of Technology Concurred By: Dr. Gary Blackwood Date Program Manager Exoplanet Exploration Program NASA/Jet Propulsion Laboratory California Institute of Technology EXOPDr.LANET Douglas Hudgins E XPLORATION PROGRAMDate Program Scientist Exoplanet Exploration Program ScienceScience Plan Mission DirectorateAppendix NASA Headquarters Karl Stapelfeldt, Program Chief Scientist Eric Mamajek, Deputy Program Chief Scientist Exoplanet Exploration Program JPL CL#19-0790 JPL Document No: 1735632 ExEP Science Plan, Rev A JPL D: 1735632 Release Date: February 15, 2019 Page 2 of 61 Approved by: Dr. Gary Blackwood Date Program Manager, Exoplanet Exploration Program Office NASA/Jet Propulsion Laboratory Dr. Douglas Hudgins Date Program Scientist Exoplanet Exploration Program Science Mission Directorate NASA Headquarters Created by: Dr. Karl Stapelfeldt Chief Program Scientist Exoplanet Exploration Program Office NASA/Jet Propulsion Laboratory California Institute of Technology Dr. Eric Mamajek Deputy Program Chief Scientist Exoplanet Exploration Program Office NASA/Jet Propulsion Laboratory California Institute of Technology This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. © 2018 California Institute of Technology. Government sponsorship acknowledged. Exoplanet Exploration Program JPL CL#19-0790 ExEP Science Plan, Rev A JPL D: 1735632 Release Date: February 15, 2019 Page 3 of 61 Table of Contents 1.
    [Show full text]
  • Optical Spectroscopic Monitoring Observations of a T Tauri Star V409
    International Journal of Astronomy & Astrophysics, 2019, *,** Published Online **** 2019 in SciRes. http://www.scirp.org/journal/**** http://dx.doi.org/10.4236/****.2014.***** Optical Spectroscopic Monitoring Observations of a T Tauri Star V409 Tau Hinako Akimoto1 and Yoichi Itoh1 1 Nishi-Harima Astronomical Observatory, Center for Astronomy, University of Hyogo, 407-2 Nishigaichi, Sayo, Sayo, Hyogo 679-5313, Japan Email: [email protected] Received **** 2019 Copyright c 2019 by author(s) and Scientific Research Publishing Inc. This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/ Abstract We report the results of optical spectroscopic monitoring observations of a T Tauri star, V409 Tau. A previous photometric study indicated that this star experienced dimming events due to the obscuration of light from the central star with a distorted circumstellar disk. We conducted medium-resolution (R ∼ 10000) spectroscopic observations with 2-m Nayuta telescope at Nishi-Harima Astronomical Observatory. Spectra were obtained in 18 nights between November 2015 and March 2016. Several absorption lines such as Ca I and Li, and the Hα emission line were confirmed in the spectra. The Ic-band magnitudes of V409 Tau changed by approximately 1 magnitude during the observation epoch. The equivalent widths of the five absorption lines are roughly constant despite changes in the Ic-band magnitudes. We conclude that the light variation of the star is caused by the obscuration of light from the central star with a distorted circumstellar disk, based on the relationship between the equivalent widths of the absorption lines and the Ic-band magnitudes.
    [Show full text]
  • Discovery of Variable X-Ray Absorption in the Ctts AA Tauri J
    A&A 462, L41–L44 (2007) Astronomy DOI: 10.1051/0004-6361:20066693 & c ESO 2007 Astrophysics Letter to the Editor Discovery of variable X-ray absorption in the cTTS AA Tauri J. H. M. M. Schmitt and J. Robrade Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany e-mail: [email protected] Received 3 November 2006 / Accepted 6 December 2006 ABSTRACT We present XMM-Newton X-ray and UV observations of the classical T Tauri star AA Tau covering almost two rotational periods where Prot ∼ 8.5 days. Clear, but uncorrelated variability is found at both wavebands. The variability observed at ∼2100 Å follows the previously known optical period. Spectral analysis of the X-ray data results in significant variability in the X-ray absorption such that the times of maximal X-ray absorption and UV extinction coincide. Placing the coronal emission in regions at low up to moderate magnetic latitudes and attribution of the variable X-ray absorption to accretion curtains and/or the disk warp provides a consistent physical picture. However, the derived X-ray absorption and optical extinction at times of maximal optical/UV brightness, i.e. outside occultation, are difficult to reconcile, requiring additional absorption in a disk wind or a peculiar dust grain distribution. Key words. X-rays: stars – stars: pre-main sequence – stars: coronae – stars: activity 1. Introduction warp leads to a partial occultation of AA Tau’s photosphere, thus causing the observed almost achromatic brightness variations. T Tauri stars (TTS) are very young low-mass stars evolving to- Polarization measurements (Ménard et al.
    [Show full text]
  • Exoplanet.Eu Catalog Page 1 # Name Mass Star Name
    exoplanet.eu_catalog # name mass star_name star_distance star_mass OGLE-2016-BLG-1469L b 13.6 OGLE-2016-BLG-1469L 4500.0 0.048 11 Com b 19.4 11 Com 110.6 2.7 11 Oph b 21 11 Oph 145.0 0.0162 11 UMi b 10.5 11 UMi 119.5 1.8 14 And b 5.33 14 And 76.4 2.2 14 Her b 4.64 14 Her 18.1 0.9 16 Cyg B b 1.68 16 Cyg B 21.4 1.01 18 Del b 10.3 18 Del 73.1 2.3 1RXS 1609 b 14 1RXS1609 145.0 0.73 1SWASP J1407 b 20 1SWASP J1407 133.0 0.9 24 Sex b 1.99 24 Sex 74.8 1.54 24 Sex c 0.86 24 Sex 74.8 1.54 2M 0103-55 (AB) b 13 2M 0103-55 (AB) 47.2 0.4 2M 0122-24 b 20 2M 0122-24 36.0 0.4 2M 0219-39 b 13.9 2M 0219-39 39.4 0.11 2M 0441+23 b 7.5 2M 0441+23 140.0 0.02 2M 0746+20 b 30 2M 0746+20 12.2 0.12 2M 1207-39 24 2M 1207-39 52.4 0.025 2M 1207-39 b 4 2M 1207-39 52.4 0.025 2M 1938+46 b 1.9 2M 1938+46 0.6 2M 2140+16 b 20 2M 2140+16 25.0 0.08 2M 2206-20 b 30 2M 2206-20 26.7 0.13 2M 2236+4751 b 12.5 2M 2236+4751 63.0 0.6 2M J2126-81 b 13.3 TYC 9486-927-1 24.8 0.4 2MASS J11193254 AB 3.7 2MASS J11193254 AB 2MASS J1450-7841 A 40 2MASS J1450-7841 A 75.0 0.04 2MASS J1450-7841 B 40 2MASS J1450-7841 B 75.0 0.04 2MASS J2250+2325 b 30 2MASS J2250+2325 41.5 30 Ari B b 9.88 30 Ari B 39.4 1.22 38 Vir b 4.51 38 Vir 1.18 4 Uma b 7.1 4 Uma 78.5 1.234 42 Dra b 3.88 42 Dra 97.3 0.98 47 Uma b 2.53 47 Uma 14.0 1.03 47 Uma c 0.54 47 Uma 14.0 1.03 47 Uma d 1.64 47 Uma 14.0 1.03 51 Eri b 9.1 51 Eri 29.4 1.75 51 Peg b 0.47 51 Peg 14.7 1.11 55 Cnc b 0.84 55 Cnc 12.3 0.905 55 Cnc c 0.1784 55 Cnc 12.3 0.905 55 Cnc d 3.86 55 Cnc 12.3 0.905 55 Cnc e 0.02547 55 Cnc 12.3 0.905 55 Cnc f 0.1479 55
    [Show full text]
  • Arxiv:2009.03398V2 [Astro-Ph.EP] 12 Sep 2020
    vDraft version September 15, 2020 Typeset using LATEX twocolumn style in AASTeX63 Physical Parameters of the Multi-Planet Systems HD 106315 and GJ 9827∗y Molly R. Kosiarek,1, z David A. Berardo,2 Ian J. M. Crossfield,3 Cesar Laguna,4 Joseph M. Akana Murphy,1, z Steve B. Howell,5 Gregory W. Henry,6 Howard Isaacson,7, 8 Lauren M. Weiss,9 Erik A. Petigura,10 Benjamin Fulton,11 Aida Behmard,12 Lea A. Hirsch,13 Johanna Teske,14 Jennifer A. Burt,15 Sean M. Mills,16 Ashley Chontos,17, z Teo Mocnik,18 Andrew W. Howard,16 Michael Werner,15 John H. Livingston,19 Jessica Krick,20 Charles Beichman,21 Varoujan Gorjian,15 Laura Kreidberg,22, 23 Caroline Morley,24 Jessie L. Christiansen,20 Farisa Y. Morales,15 Nicholas J. Scott,5 Jeffrey D. Crane,25 Lee J. Rosenthal,16 Samuel K. Grunblatt,26, 27 Ryan A. Rubenzahl,16, z Paul A. Dalba,28, x Steven Giacalone,29 Chiara Dane Villanueva,4 Qingtian Liu,4 Fei Dai,12 Michelle L. Hill,28 Malena Rice,30 Stephen R. Kane,28 Andrew W. Mayo,29, 31 | 1Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA 2Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 3Department of Physics & Astronomy, University of Kansas, 1082 Malott,1251 Wescoe Hall Dr., Lawrence, KS 66045, USA 4Department of Physics, University of California, Santa Cruz, CA 95064, USA 5NASA Ames Research Center, Moffett Field, CA 94035, USA 6Center of Excellence in Information Systems, Tennessee State University, Nashville, TN
    [Show full text]
  • Hans Moritz Günther
    page 1 of 3 Hans Moritz G¨unther - List of publications Refereed publications First author publications 16. YSOVAR: Mid-infrared Variability in the Star-forming Region Lynds 1688 H. M. G¨unther, A. M. Cody, K. R. Covey, L. A. Hillenbrand, P. Plavchan, K. Poppenhaeger, L. M. Rebull, J. R. Stauffer, S. J. Wolk, L. Allen, A. Bayo, R. A. Gutermuth, J. L. Hora, H. Y. A. Meng, M. Morales-Calder´on,J. R. Parks, Insoek Song (2014), AJ 148, 122 15. Recollimation Boundary Layers as X-Ray Sources in Young Stellar Jets H. M. G¨unther, Zhi-Yun Li, P. C. Schneider (2014), ApJ, 795, 51 14. MN Lup: X-rays from a Weakly Accreting T Tauri Star H. M. G¨unther, U. Wolter, J. Robrade, S. J. Wolk (2013), ApJ 771, 70 13. The evolution of the jet from the Herbig Ae Star HD 163296 in the last decade H. M. G¨unther, P. C. Schneider, Z.-Y. Li (2013), A&A 552, 142 12. Accretion, winds and outflows in young stars H. M. G¨unther (2013), AN 334, 67 11. IRAS 20050+2720: Anatomy of a Young Stellar Cluster H. M. G¨unther, S. J. Wolk, B. Spitzbart, R. A. Gutermuth, J. Forbrich, N. J. Wright, L. Allen, T. L. Bourke, S. T. Megeath, J. L. Pipher (2012), AJ 144, 101 10. Soft Coronal X-Rays from β Pictoris H. M. G¨unther, S. J. Wolk, J. J. Drake, C. M. Lisse,J. Robrade, J. H. M. M. Schmitt (2012), ApJ 750, 78 9. Accretion, jets and winds: High-energy emission from young stellar objects H.
    [Show full text]
  • Gliese 49: Activity Evolution and Detection of a Super-Earth? a HADES and CARMENES Collaboration
    Astronomy & Astrophysics manuscript no. Gl49b ©ESO 2020 December 4, 2020 Gliese 49: Activity evolution and detection of a super-Earth? A HADES and CARMENES collaboration M. Perger1; 2, G. Scandariato3, I. Ribas1; 2, J. C. Morales1; 2, L. Affer4, M. Azzaro5, P. J. Amado6, G. Anglada-Escudé6; 7, D. Baroch1; 2, D. Barrado8, F. F. Bauer6, V. J. S. Béjar9; 10, J. A. Caballero8, M. Cortés-Contreras8, M. Damasso11, S. Dreizler12, L. González-Cuesta9; 10, J. I. González Hernández9; 10, E. W. Guenther13, T. Henning14, E. Herrero1; 2, S.V. Jeffers12, A. Kaminski15, M. Kürster14, M. Lafarga1; 2, G. Leto3, M. J. López-González6, J. Maldonado4, G. Micela4, D. Montes16, M. Pinamonti11, A. Quirrenbach15, R. Rebolo9; 10; 17, A. Reiners12, E. Rodríguez6, C. Rodríguez-López6, J. H. M. M. Schmitt18, A. Sozzetti11, A. Suárez Mascareño9; 19, B. Toledo-Padrón9; 10, R. Zanmar Sánchez3, M. R. Zapatero Osorio20, and M. Zechmeister12 (Affiliations can be found after the references) Accepted: 11 March 2019 ABSTRACT Context. Small planets around low-mass stars often show orbital periods in a range that corresponds to the temperate zones of their host stars which are therefore of prime interest for planet searches. Surface phenomena such as spots and faculae create periodic signals in radial velocities and in observational activity tracers in the same range, so they can mimic or hide true planetary signals. Aims. We aim to detect Doppler signals corresponding to planetary companions, determine their most probable orbital configurations, and understand the stellar activity and its impact on different datasets. Methods. We analyzed 22 years of data of the M1.5 V-type star Gl 49 (BD+61 195) including HARPS-N and CARMENES spec- trographs, complemented by APT2 and SNO photometry.
    [Show full text]