From Disks to Planets: The Making of Planets and Their Early Atmospheres. An Introduction

Lämmer, H.; Blanc, Michel

doi:10.1007/978-94-024-1518-6_2

Cited by 2 publications

(18 citation statements)

References 148 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…N2 ATMOSPHERES ON EARTH-LIKE PLANETS 929 Kasting, 1993;Zahnle, 2006;Lammer et al, 2018). Then, as illustrated in Fig.…”

Section: Abiotic Magmatic Surface Interactions and Steam Atmosphere Cmentioning

confidence: 98%

“…The evolution of an Earth-like planet and its atmosphere is strongly related to various processes, for example, the planet's formation, its initial volatile and water inventory, the host star's activity controlling the escape of the planetary protoatmosphere, the evolution of the secondary atmosphere, and the planet's impact history (e.g., Halliday, 2003;Lammer et al, 2013aLammer et al, , 2018Mikhail and Sverjensky, 2014;Wordsworth, 2016;Catling and Kasting, 2017;Zerkle and Mikhail, 2017;Lammer and Blanc, 2018).…”

Section: ''mentioning

confidence: 99%

“…In the earliest stages of planet formation, protoplanetary cores can accumulate H 2 envelopes (Sekiya et al, 1980a(Sekiya et al, , 1980bSasaki and Nakazawa, 1988;Lammer and Blanc, 2018). Due to the captured nebula gas, serpentinization, and accreting chondritic material, crust and atmosphere were strongly reducing and later oxidized during the planet's life (Schaefer and Fegley, 2010).…”

Section: Abiotic Magmatic Surface Interactions and Steam Atmosphere Cmentioning

confidence: 99%

“…Due to the captured nebula gas, serpentinization, and accreting chondritic material, crust and atmosphere were strongly reducing and later oxidized during the planet's life (Schaefer and Fegley, 2010). Hydrogen is partly lost during the short very efficient thermal escape phase (''boil-off phase'') and can be completely removed due to EUV-driven hydrodynamic escape (e.g., Gillmann et al, 2009;Lammer et al, 2014Lammer et al, , 2018Johnstone et al, 2015;Fossati et al, 2017;Odert et al, 2018). After the escape of the nebular gas, the deep magma ocean on the planet's surface solidifies and thereby outgasses H 2 O and CO 2 catastrophically, so that a dense steam atmosphere evolves (Sleep, 2010).…”

Section: Abiotic Magmatic Surface Interactions and Steam Atmosphere Cmentioning

confidence: 99%

“…Since Earth developed tectonic activity, subduction of oceanic lithosphere carries oxidized surface rocks and large amounts of water into Earth's upper mantle ( Fig. 3; e.g., McCammon, 2005;Hirschmann, 2009;Lammer et al, 2018). This can locally change the redox state to favor N 2 , which is easily outgassed.…”

Section: Nitrogen Speciation In Earth's Upper Mantlementioning

confidence: 99%

See 4 more Smart Citations

The Role of N₂as a Geo-Biosignature for the Detection and Characterization of Earth-like Habitats

et al. 2019

Self Cite

View full text Add to dashboard Cite

Since the Archean, N 2 has been a major atmospheric constituent in Earth's atmosphere. Nitrogen is an essential element in the building blocks of life; therefore, the geobiological nitrogen cycle is a fundamental factor in the long-term evolution of both Earth and Earth-like exoplanets. We discuss the development of Earth's N 2 atmosphere since the planet's formation and its relation with the geobiological cycle. Then we suggest atmospheric evolution scenarios and their possible interaction with life-forms: first for a stagnant-lid anoxic world, second for a tectonically active anoxic world, and third for an oxidized tectonically active world. Furthermore, we discuss a possible demise of present Earth's biosphere and its effects on the atmosphere. Since life-forms are the most efficient means for recycling deposited nitrogen back into the atmosphere at present, they sustain its surface partial pressure at high levels. Also, the simultaneous presence of significant N 2 and O 2 is chemically incompatible in an atmosphere over geological timescales. Thus, we argue that an N 2 -dominated atmosphere in combination with O 2 on Earth-like planets within circumstellar habitable zones can be considered as a geo-biosignature. Terrestrial planets with such atmospheres will have an operating tectonic regime connected with an aerobic biosphere, whereas other scenarios in most cases end up with a CO 2 -dominated atmosphere. We conclude with implications for the search for life on Earth-like exoplanets inside the habitable zones of M to K stars.Abbreviations anammox ¼ anaerobic ammonium oxidation ELT ¼ Extremely Large Telescope GOE ¼ Great Oxidation Event 950 LAMMER ET AL.

show abstract

“…N2 ATMOSPHERES ON EARTH-LIKE PLANETS 929 Kasting, 1993;Zahnle, 2006;Lammer et al, 2018). Then, as illustrated in Fig.…”

Section: Abiotic Magmatic Surface Interactions and Steam Atmosphere Cmentioning

confidence: 98%

Section: ''mentioning

confidence: 99%

Section: Abiotic Magmatic Surface Interactions and Steam Atmosphere Cmentioning

confidence: 99%

Section: Abiotic Magmatic Surface Interactions and Steam Atmosphere Cmentioning

confidence: 99%

Section: Nitrogen Speciation In Earth's Upper Mantlementioning

confidence: 99%

See 3 more Smart Citations

The Role of N₂as a Geo-Biosignature for the Detection and Characterization of Earth-like Habitats

et al. 2019

Self Cite

View full text Add to dashboard Cite

show abstract

Exoplanetary Atmospheres: Key Insights, Challenges, and Prospects

Madhusudhan

2019

Annu. Rev. Astron. Astrophys.

312

227

View full text Add to dashboard Cite

Exoplanetary science is on the verge of an unprecedented revolution. The thousands of exoplanets discovered over the past decade have most recently been supplemented by discoveries of potentially habitable planets around nearby low-mass stars. Currently, the field is rapidly progressing towards detailed spectroscopic observations to characterise the atmospheres of these planets. While various surveys from space and ground are expected to detect numerous more exoplanets orbiting nearby stars, the imminent launch of JWST along with large groundbased facilities are expected to revolutionise exoplanetary spectroscopy. Such observations, combined with detailed theoretical models and inverse methods, provide valuable insights into a wide range of physical processes and chemical compositions in exoplanetary atmospheres. Depending on the planetary properties, the knowledge of atmospheric compositions can also place important constraints on planetary formation and migration mechanisms, geophysical processes and, ultimately, biosignatures. In the present review, we will discuss the modern and future landscape of this frontier area of exoplanetary atmospheres. We will start with a brief review of the area, emphasising the key insights gained from different observational methods and theoretical studies. This is followed by an in-depth discussion of the state-of-the-art, challenges, and future prospects in three forefront branches of the area. 2 N. Madhusudhan 6 N. Madhusudhan 28 N. Madhusudhan 42 N. Madhusudhan

show abstract

From Disks to Planets: The Making of Planets and Their Early Atmospheres. An Introduction

Cited by 2 publications

References 148 publications

The Role of N₂as a Geo-Biosignature for the Detection and Characterization of Earth-like Habitats

The Role of N₂as a Geo-Biosignature for the Detection and Characterization of Earth-like Habitats

Exoplanetary Atmospheres: Key Insights, Challenges, and Prospects

Contact Info

Product

Resources

About

From Disks to Planets: The Making of Planets and Their Early Atmospheres. An Introduction

Cited by 2 publications

References 148 publications

The Role of N2as a Geo-Biosignature for the Detection and Characterization of Earth-like Habitats

The Role of N2as a Geo-Biosignature for the Detection and Characterization of Earth-like Habitats

Exoplanetary Atmospheres: Key Insights, Challenges, and Prospects

Contact Info

Product

Resources

About

The Role of N₂as a Geo-Biosignature for the Detection and Characterization of Earth-like Habitats

The Role of N₂as a Geo-Biosignature for the Detection and Characterization of Earth-like Habitats