Sentences with phrase «terrestrial planet atmospheres»

Not exact matches

For the terrestrial planets possessing an atmosphere the increased solar flux causes similar effects.

It's possible that instead of forming as terrestrial planets in place, rocky planets orbiting their stars every few days formed further out beyond the snow line where they accreted large amounts of gas before migrating and being stripped of their atmospheres.

Owen, J. E. & Mohanty, S. Habitability of terrestrial - mass planets in the HZ of M dwarfs — I. H / He - dominated atmospheres.

As high - altitude clouds and hazes are not expected in hydrogen - dominated atmospheres around planets with such insolation15, 16, these observations further support their terrestrial and potentially habitable nature.

We focus on planets and moons orbiting stars bright enough for future atmosphere follow - up, especially Mini - to Super-Earths (rocky terrestrial planets of 0.5 - 10 Earth masses) orbiting in the «Habitable Zones» around their host stars.

Smaller terrestrial planets lose most of their atmospheres because of this accretion, but the lost gases can be replaced by outgassing from the mantle and from the subsequent impact of comets.

1:20 PM Liu - Abundance Studies of Stellar Hosts of Terrestrial Planets 1:40 PM Kitiashvili - 3D Realistic Modeling of Stellar Convection as a Tool to Study Effects of Stellar Jitter on RV Measurements 2:00 PM Crossfield - Planet Densities (invited) 2:30 PM Break and Poster Viewing 3:00 PM Guyon - Coronagraphs for Planet Detection (invited) 3:30 PM Martins - Exoplanet Reflections in the era of Giant Telescopes 3:50 PM Close - Direct Detection of Exoplanets with GMT AO: A proof of concept design for a GMT Phase A ExAO planet imager 4:10 PM Direct Imaging Discussion - Led by Jared Males 5:20 PM End of meeting for the day 5:30 PM Buses depart for Monterey Bay Aquarium 6:00 PM Conference Banquet Wednesday, September 28 7:30 - 9:00 AM Breakfast 9:00 AM Lewis - JWST - ELT Synergy (invited) 9:30 AM Greene - Characterizing exoplanet atmospheres with JWST 9:50 AM Morzinski - Breaking degeneracies in understanding fundamental exoplanet properties with ELTs 10:10 AM Break and Poster Viewing 11:00 AM Cotton - Detecting Clouds in Hot Jupiters with Linear Polarisation 11:20 AM Boss - SPlanet Densities (invited) 2:30 PM Break and Poster Viewing 3:00 PM Guyon - Coronagraphs for Planet Detection (invited) 3:30 PM Martins - Exoplanet Reflections in the era of Giant Telescopes 3:50 PM Close - Direct Detection of Exoplanets with GMT AO: A proof of concept design for a GMT Phase A ExAO planet imager 4:10 PM Direct Imaging Discussion - Led by Jared Males 5:20 PM End of meeting for the day 5:30 PM Buses depart for Monterey Bay Aquarium 6:00 PM Conference Banquet Wednesday, September 28 7:30 - 9:00 AM Breakfast 9:00 AM Lewis - JWST - ELT Synergy (invited) 9:30 AM Greene - Characterizing exoplanet atmospheres with JWST 9:50 AM Morzinski - Breaking degeneracies in understanding fundamental exoplanet properties with ELTs 10:10 AM Break and Poster Viewing 11:00 AM Cotton - Detecting Clouds in Hot Jupiters with Linear Polarisation 11:20 AM Boss - SPlanet Detection (invited) 3:30 PM Martins - Exoplanet Reflections in the era of Giant Telescopes 3:50 PM Close - Direct Detection of Exoplanets with GMT AO: A proof of concept design for a GMT Phase A ExAO planet imager 4:10 PM Direct Imaging Discussion - Led by Jared Males 5:20 PM End of meeting for the day 5:30 PM Buses depart for Monterey Bay Aquarium 6:00 PM Conference Banquet Wednesday, September 28 7:30 - 9:00 AM Breakfast 9:00 AM Lewis - JWST - ELT Synergy (invited) 9:30 AM Greene - Characterizing exoplanet atmospheres with JWST 9:50 AM Morzinski - Breaking degeneracies in understanding fundamental exoplanet properties with ELTs 10:10 AM Break and Poster Viewing 11:00 AM Cotton - Detecting Clouds in Hot Jupiters with Linear Polarisation 11:20 AM Boss - Splanet imager 4:10 PM Direct Imaging Discussion - Led by Jared Males 5:20 PM End of meeting for the day 5:30 PM Buses depart for Monterey Bay Aquarium 6:00 PM Conference Banquet Wednesday, September 28 7:30 - 9:00 AM Breakfast 9:00 AM Lewis - JWST - ELT Synergy (invited) 9:30 AM Greene - Characterizing exoplanet atmospheres with JWST 9:50 AM Morzinski - Breaking degeneracies in understanding fundamental exoplanet properties with ELTs 10:10 AM Break and Poster Viewing 11:00 AM Cotton - Detecting Clouds in Hot Jupiters with Linear Polarisation 11:20 AM Boss - Summary

And just as increased algal productivity at sea increases the emission of sulfur gases to the atmosphere, ultimately leading to more and brighter clouds over the world's oceans, so too do CO2 - induced increases in terrestrial plant productivity lead to enhanced emissions of various sulfur gases over land, where they likewise ultimately cool the planet.

The ocean, with around 38,000 gigatons (Gt) of carbon (1 gigaton = 1 billion tons), contains 16 times as much carbon as the terrestrial biosphere, that is all plant and the underlying soils on our planet, and around 60 times as much as the pre-industrial atmosphere, i.e., at a time before people began to drastically alter the atmospheric CO2 content by the increased burning of coal, oil and gas.

I read the CDIAC quote provided by Robert as; only 40 % of the additional CO2 added to the environment by manmade activities remains in the atmosphere while the balance, 60 %, has been transferred back to planet earth (oceans and terrestrial biosphere).

Wordsworth R and Pierrehumbert RT 2013: Water loss from terrestrial planets with CO2 - rich atmospheres Astrophysical J -RCB-, 778 doi: 10.1088 / 0004 - 637X / 778 / 2/154 pdf