Stellar Wind Contribution to the Origin of Water on the Surface of Oxygen-containing Minerals

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F61388955%3A_____%2F24%3A00600171" target="_blank" >RIV/61388955:_____/24:00600171 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/61388963:_____/24:00600171

Výsledek na webu

<a href="https://iopscience.iop.org/article/10.3847/1538-4357/ad77cd" target="_blank" >https://iopscience.iop.org/article/10.3847/1538-4357/ad77cd</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-4357/ad77cd" target="_blank" >10.3847/1538-4357/ad77cd</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Stellar Wind Contribution to the Origin of Water on the Surface of Oxygen-containing Minerals

Popis výsledku v původním jazyce

The origin of water and volatile compounds on planets including Earth is a hotly debated topic in planetary science. For example, many dynamic models suggest that the majority of Earth's water and volatile elements were added from an external source. The stellar wind irradiation of rocky oxygen-containing minerals results in a reaction between H+ ions and silicate minerals to produce water and OH, which could explain the presence of water in the regoliths of airless worlds such as the Moon, as well as the water abundances in asteroids. Here, we used the method of high-resolution infrared spectrometry and temperature-programmed desorption (TPD) with mass detection to observe and for the first time quantify water formation on the surfaces of oxygen-bearing minerals. We tested 14 different mineral and natural samples and observed the formation of water on their surfaces upon exposure to H+ or D+ irradiation. The samples, including two meteorite samples (RAS 445 and SAU 567), were shown to have a water adsorption capacity between 0.09 and 0.7 wt%. The adsorbed water (likely dissociatively adsorbed) remains on the surface at pressures as low as 10-9 mbar (in the TPD experiment) and temperatures as high as 600 K, which suggests a possible transfer over long distances and timescales. Our article has a general character and demonstrates that any interaction of oxygen-containing minerals with stellar radiation (H+ ions) leads to the generation of water adsorbed on the surface of the minerals. The case of the origin of water on Earth is taken as a prime example.

Název v anglickém jazyce

Stellar Wind Contribution to the Origin of Water on the Surface of Oxygen-containing Minerals

Popis výsledku anglicky

The origin of water and volatile compounds on planets including Earth is a hotly debated topic in planetary science. For example, many dynamic models suggest that the majority of Earth's water and volatile elements were added from an external source. The stellar wind irradiation of rocky oxygen-containing minerals results in a reaction between H+ ions and silicate minerals to produce water and OH, which could explain the presence of water in the regoliths of airless worlds such as the Moon, as well as the water abundances in asteroids. Here, we used the method of high-resolution infrared spectrometry and temperature-programmed desorption (TPD) with mass detection to observe and for the first time quantify water formation on the surfaces of oxygen-bearing minerals. We tested 14 different mineral and natural samples and observed the formation of water on their surfaces upon exposure to H+ or D+ irradiation. The samples, including two meteorite samples (RAS 445 and SAU 567), were shown to have a water adsorption capacity between 0.09 and 0.7 wt%. The adsorbed water (likely dissociatively adsorbed) remains on the surface at pressures as low as 10-9 mbar (in the TPD experiment) and temperatures as high as 600 K, which suggests a possible transfer over long distances and timescales. Our article has a general character and demonstrates that any interaction of oxygen-containing minerals with stellar radiation (H+ ions) leads to the generation of water adsorbed on the surface of the minerals. The case of the origin of water on Earth is taken as a prime example.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10403 - Physical chemistry

Projekt

<a href="/cs/project/LM2023066" target="_blank" >LM2023066: Nanomateriály a nanotechnologie pro ochranu životního prostředí a udržitelnou budoucnost</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2024

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astrophysical Journal

ISSN

0004-637X

e-ISSN

1538-4357

Svazek periodika

975

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

12

Strana od-do

25

Kód UT WoS článku

001339482400001

EID výsledku v databázi Scopus

2-s2.0-85207702931