New experimental observations on the anhydrous solidus for peridotite KLB‐1

Herzberg, Claude; Raterron, Paul; Zhang, Jianzhong

doi:10.1029/2000gc000089

Cited by 145 publications

(124 citation statements)

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“…Our melt model has been described in detail in Stamenković & Breuer (2014) and for the melting temperature in the upper mantle (where the melt that drives outgassing is produced) our model uses the solidus for Earth-like peridotite, T melt,peridotite . This T melt,peridotite is obtained by fitting the data from Herzberg et al (2000), Zerr et al (1998), andFiquet et al (2010; see Equation (7) in Stamenković & Breuer 2014). Water can have a significant effect on reducing the solidus temperature of mantle rock (e.g., Asimow et al 2004;Aubaud et al 2004;Hirschmann 2006;Grove et al 2009).…”

Section: Methodsmentioning

confidence: 99%

Temporal Evolution of the High-energy Irradiation and Water Content of TRAPPIST-1 Exoplanets

et al. 2017

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The ultracool dwarf star TRAPPIST-1 hosts seven Earth-size transiting planets, some of which could harbor liquid water on their surfaces. Ultraviolet observations are essential to measuring their high-energy irradiation and searching for photodissociated water escaping from their putative atmospheres. Our new observations of the TRAPPIST-1 Lyα line during the transit of TRAPPIST-1c show an evolution of the star emission over three months, preventing us from assessing the presence of an extended hydrogen exosphere. Based on the current knowledge of the stellar irradiation, we investigated the likely history of water loss in the system. Planets b to d might still be in a runaway phase, and planets within the orbit of TRAPPIST-1g could have lost more than 20 Earth oceans after 8 Gyr of hydrodynamic escape. However, TRAPPIST-1e to h might have lost less than three Earth oceans if hydrodynamic escape stopped once they entered the habitable zone (HZ). We caution that these estimates remain limited by the large uncertainty on the planet masses. They likely represent upper limits on the actual water loss because our assumptions maximize the X-rays to ultraviolet-driven escape, while photodissociation in the upper atmospheres should be the limiting process. Late-stage outgassing could also have contributed significant amounts of water for the outer, more massive planets after they entered the HZ. While our results suggest that the outer planets are the best candidates to search for water with the JWST, they also highlight the need for theoretical studies and complementary observations in all wavelength domains to determine the nature of the TRAPPIST-1 planets and their potential habitability.

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Section: Methodsmentioning

confidence: 99%

Temporal Evolution of the High-energy Irradiation and Water Content of TRAPPIST-1 Exoplanets

et al. 2017

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“…The eclogitic composition "G2" is even more discrepant from the peridotite solidi, as recorded the "G2" solidus at 2 and 3 GPa respectively, to be 190±25ºC and 170±25ºC cooler than the depleted peridotite solidus [Herzberg et al, 2000;Walter, 1998]. Using the peridotite solidus parameterization of Hirschmann , which is based on experimental peridotite melting data [Walter, 1998], this difference in temperature equates to an eclogite lithology 60% molten by the time the 3 GPa 'dry' peridotite solidus is reached .…”

Section: Bimodal Meltingmentioning

confidence: 99%

The influence of ridge geometry at the ultraslow-spreading Southwest Indian Ridge (9º-25ºE) : basalt composition sensitivity to variations in source and process

Standish¹

2006

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Between 9º-25º E on the ultraslow-spreading Southwest Indian Ridge lie two sharply contrasting supersegments. One 630 km long supersegment erupts N-MORB that is progressively enriched in incompatible element concentrations from east to west. The second 400 km long supersegment contains three separate volcanic centers erupting E-MORB and connected by long amagmatic accretionary segments, where mantle is emplaced directly to the seafloor with only scattered N-MORB and E-MORB erupted. Rather than a major break in mantle composition at the discontinuity between the supersegments, this sharp contrast in geometry, physiography, and chemistry reflects "source" versus "process" dominated generation of basalt.Robust along-axis correlation of ridge characteristics (i.e. morphology, upwelling rate, lithospheric thickness), basalt chemistry, and crustal thickness (estimated from gravity) provides a unique opportunity to compare the influence of spreading geometry and rate on MORB generation. What had not been well established until now is the importance of melting processes rather than source at spreading rates < 20 mm/yr. Along the orthogonally spreading supersegment (14 mm/yr) moderate degrees of partial melting effectively sample the bulk mantle source, while on the obliquely spreading supersegment (7-14 mm/yr) suppression of mantle melting to low degrees means that the bulk source is not uniformly sampled, and thus "process" rather than "source" dominates melt chemistry. AcknowledgementsThere are so many people to thank when reaching a milestone such as this, so let me start with those that have had the most recent impact on this accomplishment, my thesis committee; Henry Dick, Stan Hart, Ken Sims, Fred Frey, Anton le Roex, Mark Kurz, Jian Lin, and my thesis defense chairperson, Hans Schouten. With both Hans and Jian I have gained a new appreciation for and understanding of real-time seagoing geophysics, and I think all four of us (including Henry) have witnessed some pretty amazing human efforts and as a result grown together as people and scientists during the many days bouncing around the South Atlantic. Mark's analytical expertise, continuing support and encouraging words, and attention to detail, has kept my path over the last 6 years straight and narrow, and in the right direction. Anton has been a great source of information both regarding trace elements and more importantly the SW Indian Ridge. As one of the first geochemists to study the South Atlantic spreading ridges in detail, his early work through the 80's and 90's set the bar (and quite a high bar it was) for which all of my work will be gauged. It is a shame that our schedules did not coincide so that he could be here at WHOI for the defense, but I know much discussion will come from my work. Learning trace element geochemistry from Fred Frey was special. Fred's ability to get back to the basics and stress the importance to understanding "why" in the most fundamental terms is important in geochemistry. I very much appreciated his willingness to ...

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“…Different parameterizations for the solidus of peridotite have been derived from melting experiments (McKenzie and Bickle, 1988;Takahashi, 1990;Zhang and Herzberg, 1994;Herzberg et al, 2000;Hirschmann, 2000;Katz et al, 2003). Melting models are summarized in Fig.…”

Section: Parametersmentioning

confidence: 99%

Crustal recycling, mantle dehydration, and the thermal evolution of Mars

Morschhauser

Grott

Breuer

2011

Icarus

129

167

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Please cite this article as: Morschhauser, A., Grott, M., Breuer, D., Crustal recycling, mantle dehydration, and the thermal evolution of Mars, Icarus (2010), doi: 10.1016/j.icarus.2010 This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain.Crustal recycling, mantle dehydration, and the thermal evolution of Mars Mars would then be driven by the extraction of a primordial crust after core formation, cooling the mantle to temperatures close to the peridotite solidus. According to this scenario, the second stage of global crust formation took place over a more extended period of time, waning at around 3500 Myr b.p., and was driven by heat produced by the decay of radioactive elements. Present-day volcanism would then be driven by mantle plumes originating at the core-mantle boundary under regions of locally thickened, thermally insulating crust. Water extraction from the mantle was found to be 1 relatively efficient and close to 40 percent of the total inventory was lost from the mantle in most models. Assuming an initial mantle water content of 100 ppm and that 10% of the extracted water is supplied to the surface, this amount is equivalent to a 15 m thick global surface layer, suggesting that volcanic outgassing of H 2 O could have significantly influenced the early Martian climate and increased the planet's habitability.

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New experimental observations on the anhydrous solidus for peridotite KLB‐1

Cited by 145 publications

References 22 publications

Temporal Evolution of the High-energy Irradiation and Water Content of TRAPPIST-1 Exoplanets

Temporal Evolution of the High-energy Irradiation and Water Content of TRAPPIST-1 Exoplanets

The influence of ridge geometry at the ultraslow-spreading Southwest Indian Ridge (9º-25ºE) : basalt composition sensitivity to variations in source and process

Crustal recycling, mantle dehydration, and the thermal evolution of Mars

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