WSO-UV—ultraviolet mission for the next decade

Шустов, Б. М.; Sachkov, Mikhail; Castro, Ana Inés Gómez de; Huang, M.; Werner, K.; Kappelmann, N.; Pagano, I.

doi:10.1007/978-90-481-3006-1_32

Cited by 12 publications

(12 citation statements)

References 3 publications

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“…Color images available online at www.liebertonline.com/ast contribution of ENAs to the stellar XUV flux is beyond the scope of this particular work but is in progress for a followup study in the near future. We note also that ENA clouds near the terrestrial exoplanets within orbits around M dwarfs might be observable in the stellar Lyman-a line by the Hubble Space Telescope and in higher resolution beyond the geocorona in the near future by the World Space Observatory-UV (Shustov et al, 2009;Lammer et al, 2011b).…”

Section: Input Parameters and Modeling Resultsmentioning

confidence: 78%

XUV-Exposed, Non-Hydrostatic Hydrogen-Rich Upper Atmospheres of Terrestrial Planets. Part II: Hydrogen Coronae and Ion Escape

et al. 2013

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We studied the interactions between the stellar wind plasma flow of a typical M star, such as GJ 436, and the hydrogen-rich upper atmosphere of an Earth-like planet and a ''super-Earth'' with a radius of 2 R Earth and a mass of 10 M Earth , located within the habitable zone at *0.24 AU. We investigated the formation of extended atomic hydrogen coronae under the influences of the stellar XUV flux (soft X-rays and EUV), stellar wind density and velocity, shape of a planetary obstacle (e.g., magnetosphere, ionopause), and the loss of planetary pickup ions on the evolution of hydrogen-dominated upper atmospheres. Stellar XUV fluxes that are 1, 10, 50, and 100 times higher compared to that of the present-day Sun were considered, and the formation of high-energy neutral hydrogen clouds around the planets due to the charge-exchange reaction under various stellar conditions was modeled. Charge-exchange between stellar wind protons with planetary hydrogen atoms, and photoionization, lead to the production of initially cold ions of planetary origin. We found that the ion production rates for the studied planets can vary over a wide range, from *1.0 · 10 25 s -1 to *5.3 · 10 30 s -1 , depending on the stellar wind conditions and the assumed XUV exposure of the upper atmosphere. Our findings indicate that most likely the majority of these planetary ions are picked up by the stellar wind and lost from the planet. Finally, we estimated the long-time nonthermal ion pickup escape for the studied planets and compared them with the thermal escape. According to our estimates, nonthermal escape of picked-up ionized hydrogen atoms over a planet's lifetime within the habitable zone of an M dwarf varies between *0.4 Earth ocean equivalent amounts of hydrogen (EO H ) to < 3 EO H and usually is several times smaller in comparison to the thermal atmospheric escape rates.

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Section: Input Parameters and Modeling Resultsmentioning

confidence: 78%

XUV-Exposed, Non-Hydrostatic Hydrogen-Rich Upper Atmospheres of Terrestrial Planets. Part II: Hydrogen Coronae and Ion Escape

et al. 2013

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“…The WSO-UV's core program will focus also on exoplanetary atmospheres and astrochemistry in the presence of strong UV radiation fields (Gómez de Castro et al, 2009;Shustov et al, 2009). In Lammer et al (2011b) it was shown that it may be possible to observe transits in UV of Earth-size exoplanets with extended hydrogen coronae if they orbit around small stars.…”

Section: Testing Atmosphere Evolution Scenarios Via Uv-transit Observmentioning

confidence: 99%

Variability of solar/stellar activity and magnetic field and its influence on planetary atmosphere evolution

et al. 2012

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It is shown that the evolution of planetary atmospheres can only be understood if one recognizes the fact that the radiation and particle environment of the Sun or a planet's host star were not always on the same level as at present. New insights and the latest observations and research regarding the evolution of the solar radiation, plasma environment and solar/stellar magnetic field derived from the observations of solar proxies with different ages will be given. We show that the extreme radiation and plasma environments of the young Sun/stars have important implications for the evolution of planetary atmospheres and may be responsible for the fact that planets with low gravity like early Mars most likely never build up a dense atmosphere during the first few 100 Myr after their origin. Finally we present an innovative new idea on how hydrogen clouds and energetic neutral atom (ENA) observations around transiting Earth-like exoplanets by space observatories such as the WSO-UV, can be used for validating the addressed atmospheric evolution studies. Such observations would enhance our understanding on the impact on the activity of the young Sun on the early atmospheres of Venus, Earth, Mars and other Solar System bodies as well as exoplanets.

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“…The three optical trains are not used for simultaneous observation, but in sequential mode. This is managed by satellite motion with a pointing stability requirement of 0.1 arcsec to be monitored by three Fine Guidance Sensors (see Shustov et al 2009Shustov et al , 2011. In addition to this, in the UVES and VUVES branches UBV photometers for general characterization of the observed objects as well as for object position monitoring on the entrance slits were foreseen.…”

Section: Previous Design Of Wso-uv Spectrographsmentioning

confidence: 99%

Optical layouts of the WSO-UV spectrographs

Панчук

Yushkin

Фатхуллин

et al. 2014

Astrophys Space Sci

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World Space Observatory-Ultraviolet project is an international space observatory for spectroscopy and imaging in 115-310 nm spectral range. Significant progress in the CCD development allows to use the back illuminated CCD detectors with anti-reflection coating for observations in this ultraviolet domain instead of MCP detectors. This detector change was one of the main reason for significant correction of layouts of all three WSO-UV spectrographs. In this paper we present the final optical layouts that are now being realized in the WUVS instrument. The using of implemented technological changes in optical layout allows to keep main requirements to WSO-UV spectrographs.

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WSO-UV—ultraviolet mission for the next decade

Cited by 12 publications

References 3 publications

XUV-Exposed, Non-Hydrostatic Hydrogen-Rich Upper Atmospheres of Terrestrial Planets. Part II: Hydrogen Coronae and Ion Escape

XUV-Exposed, Non-Hydrostatic Hydrogen-Rich Upper Atmospheres of Terrestrial Planets. Part II: Hydrogen Coronae and Ion Escape

Variability of solar/stellar activity and magnetic field and its influence on planetary atmosphere evolution

Optical layouts of the WSO-UV spectrographs

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