Evolution of the Solar Activity over Time and Effects on Planetary Atmospheres: I. High-energy Irradiances (1-1700 A)

Abstract

We report on the results of the Sun in Time multi-wavelength program (X-rays to the UV) of solar analogs with ages covering ~0.1-7 Gyr. The chief science goals are to study the solar magnetic dynamo and to determine the radiative and magnetic properties of the Sun during its evolution across the main sequence. The present paper focuses on the latter goal, which has the ultimate purpose of providing the spectral irradiance evolution of solar-type stars to be used in the study and modeling of planetary atmospheres. The results from the Sun in Time program suggest that the coronal X-ray-EUV emissions of the young main-sequence Sun were ~100-1000 times stronger than those of the present Sun. Similarly, the transition region and chromospheric FUV-UV emissions of the young Sun are expected to be 20-60 and 10-20 times stronger, respectively, than at present. When considering the integrated high-energy emission from 1 to 1200 A, the resulting relationship indicates that the solar high-energy flux was about 2.5 times the present value 2.5 Gyr ago and about 6 times the present value about 3.5 Gyr ago (when life supposedly arose on Earth). The strong radiation emissions inferred should have had major influences on the thermal structure, photochemistry, and photoionization of planetary atmospheres and also played an important role in the development of primitive life in the Solar System. Some examples of the application of the Sun in Time results on exoplanets and on early Solar System planets are discussed.

20 pages, 8 figures, accepted for publication in ApJ

References in corpus (1)

• Initial Results from the Palomar Adaptive Optics Survey of Young Solar-Type Stars: a Brown Dwarf and Three Stellar Companions

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• Atmospheric collapse and re-inflation through impacts for terrestrial planets around M dwarfs
• Nitrogen Loss from Pluto's Birth to the Present Day via Atmospheric Escape, Photochemical Destruction, and Impact Erosion
• Densities of small planets around the M dwarfs TOI-4336 A and TOI-4342 with ESPRESSO: Three sub-Neptunes, one super-Earth, and a Neptune-mass candidate
• The long-term evolution of stellar activity
• Escape and evolution of Mars' CO2 atmosphere: Influence of suprathermal atoms
• High-resolution spectropolarimetric of k Cet: A proxy for the young Sun
• Quantitative Nonequilibrium Pathway from Fundamental Physics to the Emergence and Persistence of Exoplanetary Biospheres
• Evolution and Observable Properties of Rocky Planet Atmospheres
• Biological Damage due to Photospheric, Chromospheric and Flare Radiation in the Environments of Main-Sequence Stars
• An Adolescent and Near-Resonant Planetary System Near the End of Photoevaporation
• eROSITA - Nearby Young Stars in X-rays
• The SOL $\text{(Solar Origin and Life)}$ Project: Detailed characterization of candidates for the ZAMS and Subgiant stages
• Inversion of Hydrogen-rich Atmosphere and Water Content for GJ 486b
• Survival of Primordial Planetary Atmospheres: Mass Loss from Temperate Terrestrial Planets
• Stellar activity cycles and contribution of the deep layers knowledge
• Setting the Stage: The Early History of the Solar System
• An Evolving Cosmic Shoreline and Sandbar Bounding the Rocky Airless Valley
• Mars: new insights and unresolved questions
• The Solar Twin Planet Search: IV. The Sun as a typical rotator and evidence for a new rotational braking law for Sun-like stars
• TFAW survey II: 6 Newly Validated Planets and 13 Planet Candidates from K2
• Chandra X-ray Observations of V830 Tau: A T Tauri Star Hosting an Evanescent Planet
• Simulated Effects of Radioactive Elements on Magnetic Evolution and Atmospheric Mass Loss of Earth-like Planets
• Probing habitable regions with SRG/eROSITA