Jupiter's auroral-related stratospheric heating and chemistry II: Analysis of IRTF-TEXES spectra measured in December 2014

ICARUS 300 (2018) 305-326

JA Sinclair, GS Orton, TK Greathouse, LN Fletcher, JI Moses, V Hue, PGJ Irwin

Ice-shelf damming in the glacial Arctic Ocean: dynamical regimes of a basin-covering kilometre-thick ice shelf

CRYOSPHERE 11 (2017) 1745-1765

J Nilsson, M Jakobsson, C Borstad, N Kirchner, G Bjork, RT Pierrehumbert, C Stranne

On the energy dissipation rate at the inner edge of circumbinary discs


C Terquem, JCB Papaloizou

On the formation of planetary systems in photoevaporating transition discs


C Terquem

Jupiter's North Equatorial Belt expansion and thermal wave activity ahead of Juno's arrival


LN Fletcher, GS Orton, JA Sinclair, P Donnelly, H Melin, JH Rogers, TK Greathouse, Y Kasaba, T Fujiyoshi, TM Sato, J Fernandes, PGJ Irwin, RS Giles, AA Simon, MH Wong, M Vedovato

Ammonia in Jupiter's Troposphere From High-Resolution 5 μm Spectroscopy

Geophysical Research Letters 44 (2017) 10-844

RS Giles, LN Fletcher, PGJ Irwin, GS Orton, JA Sinclair

©2017. American Geophysical Union. All Rights Reserved. Jupiter's tropospheric ammonia (NH 3 ) abundance is studied using spatially resolved 5 μm observations from the cryogenic high-resolution infrared spectrograph (CRIRES) at the European Southern Observatory's Very Large Telescope. The high-resolving power (R = 96,000) allows the line shapes of three NH 3 absorption features to be resolved. We find that within the 1–4 bar pressure range, the NH 3 abundance decreases with altitude. The instrument slit was aligned north-south along Jupiter's central meridian, allowing us to search for latitudinal variability. There is considerable uncertainty in the large-scale latitudinal variability, as the increase in cloud opacity in zones compared to belts can mask absorption features. However, we do find evidence for a strong NH 3 enhancement at 4–6°N, consistent with a localized “ammonia plume” on the southern edge of Jupiter's North Equatorial Belt.

D/H Ratios on Saturn and Jupiter from Cassini CIRS


JDR Pierel, CA Nixon, E Lellouch, LN Fletcher, GL Bjoraker, RK Achterberg, B Bezard, BE Hesman, PGJ Irwin, FM Flasar

CoRoT 223992193: Investigating the variability in a low-mass, pre-main sequence eclipsing binary with evidence of a circumbinary disk


E Gillen, S Aigrain, C Terquem, J Bouvier, SHP Alencar, D Gandolfi, J Stauffer, A Cody, L Venuti, P Viana Almeida, G Micela, F Favata, HJ Deeg

The thermal structure of the Venus atmosphere: Intercomparison of Venus Express and ground based observations of vertical temperature and density profiles

ICARUS 294 (2017) 124-155

SS Limaye, S Lebonnois, A Mahieux, M Paetzold, S Bougher, S Bruinsma, S Chamberlain, RT Clancy, J-C Gerard, G Gilli, D Grassi, R Haus, M Herrmann, T Imamura, E Kohler, P Krause, A Migliorini, F Montmessin, C Pere, M Persson, A Piccialli, M Rengel, A Rodin, B Sandor, M Sornig, H Svedhem, S Tellmann, P Tanga, AC Vandaele, T Widemann, CF Wilson, I Mueller-Wodarg, L Zasova

Dynamical models to explain observations with SPHERE in planetary systems with double debris belts

ArXiv e-prints (2017)

C Lazzoni, S Desidera, F Marzari, A Boccaletti, M Langlois, D Mesa, R Gratton, Q Kral, N Pawellek, J Olofsson, M Bonnefoy, G Chauvin, AM Lagrange, A Vigan, E Sissa, J Antichi, H Avenhaus, A Baruffolo, JL Baudino, A Bazzon, JL Beuzit, B Biller, M Bonavita, W Brandner, P Bruno, E Buenzli, F Cantalloube, E Cascone, A Cheetham, RU Claudi, M Cudel, S Daemgen, V De Caprio, P Delorme, D Fantinel, G Farisato, M Feldt, R Galicher, C Ginski, J Girard, E Giro, M Janson, J Hagelberg, T Henning, S Incorvaia, M Kasper, T Kopytova, J Lannier, H LeCoroller, L Lessio, R Ligi, AL Maire, F Ménard, M Meyer, J Milli, D Mouillet, S Peretti, C Perrot, D Rouan, M Samland, B Salasnich, G Salter, T Schmidt, S Scuderi, E Sezestre, M Turatto, S Udry, F Wildi, A Zurlo

Mapping Vinyl Cyanide and Other Nitriles in Titan's Atmosphere Using ALMA


JC-Y Lai, MA Cordiner, CA Nixon, RK Achterberg, EM Molter, NA Teanby, MY Palmer, SB Chamley, JE Lindberg, Z Kisiel, MJ Mumma, PGJ Irwin

Sulfur dioxide in the Venus atmosphere: I. Vertical distribution and variability

ICARUS 295 (2017) 16-33

AC Vandaele, O Korablev, D Belyaev, S Chamberlain, D Evdokimova, T Encrenaz, L Esposito, KL Jessup, F Lefevre, S Limaye, A Mahieux, E Marcq, FP Mills, F Montmessin, CD Parkinson, S Robert, T Roman, B Sandor, A Stolzenbach, C Wilson, V Wilquet

Sulfur dioxide in the Venus Atmosphere: II. Spatial and temporal variability

ICARUS 295 (2017) 1-15

AC Vandaele, O Korablev, D Belyaev, S Chamberlain, D Evdokimova, T Encrenaz, L Esposito, KL Jessup, F Lefevre, S Limaye, A Mahieux, E Marcq, FP Mills, F Montmessin, CD Parkinson, S Robert, T Roman, B Sandor, A Stolzenbach, C Wilson, V Wilquet

Discovery of a warm, dusty giant planet around HIP 65426

Astronomy & Astrophysics 605 (2017) L9-L9

G Chauvin, S Desidera, A-M Lagrange, A Vigan, R Gratton, M Langlois, M Bonnefoy, J-L Beuzit, M Feldt, D Mouillet, M Meyer, A Cheetham, B Biller, A Boccaletti, V D’Orazi, R Galicher, J Hagelberg, A-L Maire, D Mesa, J Olofsson, M Samland, TOB Schmidt, E Sissa, M Bonavita, B Charnay, M Cudel, S Daemgen, P Delorme, P Janin-Potiron, M Janson, M Keppler, H Le Coroller, R Ligi, GD Marleau, S Messina, P Mollière, C Mordasini, A Müller, S Peretti, C Perrot, L Rodet, D Rouan, A Zurlo, C Dominik, T Henning, F Menard, H-M Schmid, M Turatto, S Udry, F Vakili, L Abe, J Antichi, A Baruffolo, P Baudoz, J Baudrand, P Blanchard, A Bazzon, T Buey, M Carbillet, M Carle, J Charton, E Cascone, R Claudi, A Costille, A Deboulbe, V De Caprio, K Dohlen, D Fantinel, P Feautrier, T Fusco, P Gigan, E Giro, D Gisler, L Gluck, N Hubin, E Hugot, M Jaquet, M Kasper, F Madec, Y Magnard, P Martinez, D Maurel, D Le Mignant, O Möller-Nilsson, M Llored, T Moulin, A Origné, A Pavlov, D Perret, C Petit, J Pragt, P Puget, P Rabou, J Ramos, R Rigal, S Rochat, R Roelfsema, G Rousset, A Roux, B Salasnich, J-F Sauvage, A Sevin, C Soenke, E Stadler, M Suarez, L Weber, F Wildi, S Antoniucci, J-C Augereau, J-L Baudino, W Brandner, N Engler, J Girard, C Gry, Q Kral, T Kopytova, E Lagadec, J Milli, C Moutou, J Schlieder, J Szulágyi, C Thalmann, Z Wahhaj

Orbiting a binary: SPHERE characterisation of the HD 284149 system

ArXiv e-prints (2017)

M Bonavita, V D Orazi, D Mesa, C Fontanive, S Desidera, S Messina, S Daemgen, R Gratton, A Vigan, M Bonnefoy, A Zurlo, J Antichi, H Avenhaus, A Baruffolo, JL Baudino, JL Beuzit, A Boccaletti, P Bruno, T Buey, M Carbillet, E Cascone, G Chauvin, RU Claudi, V De Caprio, D Fantinel, G Farisato, M Feldt, R Galicher, E Giro, C Gry, J Hagelberg, S Incorvaia, M Janson, M Jaquet, AM Lagrange, M Langlois, J Lannier, H Le Coroller, L Lessio, R Ligi, AL Maire, F Menard, C Perrot, S Peretti, C Petit, J Ramos, A Roux, B Salasnich, G Salter, M Samland, S Scuderi, J Schlieder, M Surez, M Turatto, L Weber

Observational evidence against strongly stabilizing tropical cloud feedbacks


IN Williams, RT Pierrehumbert

ALMA detection and astrobiological potential of vinyl cyanide on Titan.

Science advances 3 (2017) e1700022-

MY Palmer, MA Cordiner, CA Nixon, SB Charnley, NA Teanby, Z Kisiel, PGJ Irwin, MJ Mumma

Recent simulations have indicated that vinyl cyanide is the best candidate molecule for the formation of cell membranes/vesicle structures in Titan's hydrocarbon-rich lakes and seas. Although the existence of vinyl cyanide (C2H3CN) on Titan was previously inferred using Cassini mass spectrometry, a definitive detection has been lacking until now. We report the first spectroscopic detection of vinyl cyanide in Titan's atmosphere, obtained using archival data from the Atacama Large Millimeter/submillimeter Array (ALMA), collected from February to May 2014. We detect the three strongest rotational lines of C2H3CN in the frequency range of 230 to 232 GHz, each with >4σ confidence. Radiative transfer modeling suggests that most of the C2H3CN emission originates at altitudes of ≳200 km, in agreement with recent photochemical models. The vertical column densities implied by our best-fitting models lie in the range of 3.7 × 1013 to 1.4 × 1014 cm-2. The corresponding production rate of vinyl cyanide and its saturation mole fraction imply the availability of sufficient dissolved material to form ~107 cell membranes/cm3 in Titan's sea Ligeia Mare.

Reconstructing Climate from Glaciers

Annual Review of Earth and Planetary Sciences 45 (2017) 649-680

AN Mackintosh, BM Anderson, RT Pierrehumbert

Copyright © 2017 by Annual Reviews. All rights reserved. Glaciers offer the potential to reconstruct past climate over timescales from decades to millennia. They are found on nearly every continent, and at the Last Glacial Maximum, glaciers were larger in all regions on Earth. The physics of glacier-climate interaction are relatively well understood, and glacier models can be used to reconstruct past climate from geological evidence of past glacier extent. This can lead to significant insights regarding past, present, and future climate. For example, glacier modeling has demonstrated that the near-ubiquitous global pattern of glacier retreat during the last few centuries resulted from a global-scale climate warming of ∼1°C, consistent with instrumental data and climate proxy records. Climate reconstructions from glaciers have also demonstrated that the tropics were colder at the Last Glacial Maximum than was originally inferred from sea surface temperature reconstructions. Future efforts to reconstruct climate from glaciers may provide new constraints on climate sensitivity to CO2 forcing, polar amplification of climate change, and more.



JK Barstow, S Aigrain, PGJ Irwin, DK Sing

Rayleigh scattering in the transmission spectrum of HAT-P-18b


J Kirk, PJ Wheatley, T Louden, AP Doyle, I Skillen, J McCormac, PGJ Irwin, R Karjalainen