X‐ray views of our solar system
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Abstract The solar system comprises a relatively small number of X‐ray emitting objects, which are associated with a variety of physical emission processes: we can explore them with good spatial and temporal precision at relatively local distances, and in situ as well, unlike the rest of the Universe. Moreover, from the study of the solar system, we can gather insights into extra‐solar planets too. This article offers a review of our current knowledge of the X‐ray properties of bodies in our solar system, of the physical processes leading to X‐ray emissions, and of recent breakthrough discoveries brought about by space probes providing remote imaging as well as in situ measurements. In the long term, the next generation of Earth‐bound X‐ray observatories and the possibility of in situ X‐ray measurements, that is, by X‐ray telescopes onboard spacecraft visiting the planets, will underpin the next giant leap in discovery space.We report results of the first search specifically targeting short-timescale X-ray flares from low-mass X-ray binaries in an early-type galaxy. A new method for flare detection is presented. In NGC 4697, the nearest, optically luminous, X-ray faint elliptical galaxy, 3 out of 157 sources are found to display flares at >99.95% probability, and all show more than one flare. Two sources are coincident with globular clusters and show flare durations and luminosities similar to (but larger than) Type-I X-ray superbursts found in Galactic neutron star (NS) X-ray binaries (XRBs). The third source shows more extreme flares. Its flare luminosity (~6E39 erg/s) is very super-Eddington for an NS and is similar to the peak luminosities of the brightest Galactic black hole (BH) XRBs. However, the flare duration (~70 s) is much shorter than are typically seen for outbursts reaching those luminosities in Galactic BH sources. Alternative models for the flares are considered.
Flare
Flare star
Black hole (networking)
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There are two competing concepts for the Terrestrial Planet Finder (TPF) mission, one which involves a single spacecraft, and another comprised of a five craft formation. In addition, there are several propulsi on options under consideration. Unique contamination issues affect the formation flying concept due to the close proximity of the spacecraft. Select surfaces must be maintained at the low temperature of 40 K. There is concern that propellant expelled fr om one craft will condense on the cryogenic surfaces of a neighboring craft, adversely affecting performance and the integrity of the observational data. The condensation properties of warm argon , krypton, and xenon g ases upon a cryogenically -chilled quar tz crystal microbalance were characterized at a range of temperatures and p ressures. Initial heats of adsorption were calculated and used to calibrate a simple model that inputs a few simple parameters and outputs a residence time for a given gas particle . This residence time is used to make an estimate of adsorption rate and the maximal level of gas adsorption, as well as the time required to evaporate to an acceptable level of coverage once the thrusters are shut down . The model aims to aid in the sele ction of an appropriate propulsion system and propellant gas for the TPF spacecraft.
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This chapter contains sections titled: Introduction Conditions for the Development of Life The Development of Life on Earth Geometrical and Physical Considerations Emissions from Oxygen Absorption by Oxygen What Can We Learn from Observations in the Solar System? Conclusions
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This concluding chapter discusses some of the lessons that can be learned from studying the planets and planetary climates. It first considers the general principles that turned out to be right; for example, size and distance from the Sun matter. The larger objects are able to hold on to their atmospheres better than the small objects. The outer solar system is hydrogen rich and the inner solar system is oxygen rich; as one moves away from the Sun different substances take on different roles. There are also assumptions that proved inaccurate; such was the case for Venus, Mars, and the moons of the giant planets. The chapter also asks whether the study of planetary climates provides lessons for Earth, whether the study of planets has informed us about the likelihood of extraterrestrial life, and whether it has made the development of extraterrestrial life seem more likely.
Extraterrestrial Life
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Giant planet
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Abstract Planets Everywhere and the Search for Extraterrestrial Life begins with an overview of the types of exoplanets that have been detected so far beyond our Solar System. Statistical studies provide information about their distances from their parent stars, their masses, radii, and other characteristics. Exoplanets also inform our understanding of our Solar System. Models of planetary system formation that include the migration of planets due to the scattering of smaller planetary system bodies and orbital resonances have been developed. Of course, all physical laws must be obeyed, and all evidence must be included. The chapter and Part II conclude with the consideration of possible life beyond Earth. With evidence of amino acids and other complex molecules throughout the Solar System and in interstellar space, is it possible that sophisticated molecules like RNA and DNA could form elsewhere? Drake’s equation and the search for extraterrestrial intelligence is also explored.
Extraterrestrial Life
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Dwarf planet
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This chapter describes how the first found exoplanets presented puzzles: they orbited where they should not have formed or where they could not have survived the death of their stars. The Solar System had its own puzzles to add: Mars is smaller than expected, while Venus, Earth, and Mars had more water—at least at one time—than could be understood. This chapter shows how astronomers worked through the combination of these puzzles: now we appreciate that planets can change their orbits, scatter water-bearing asteroids about, steal material from growing planets, or team up with other planets to stabilize their future. The special history of Jupiter and Saturn as a pair bringing both destruction and water to Earth emerged from the study of seventeenth-century resonant clocks, from the water contents of asteroids, and from experiments with supercomputers imposing the laws of physics on virtual worlds.
Liquid water
Jupiter (rocket family)
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The solar system has very strong relationship with human. All the factors in it creates the distinctive circumstances for all life on Earth to survive. This study picks two planets in the solar system, i.e., Mercury and Venus, to discuss and compare on three features from the perspective of formation, atmosphere and habitability. According to the analysis, either planet is suitable for life’s existence or human’s residence based on the state-of-art techniques. To be specific, Mercury’s formation is still a problem to be solved while Venus’ is much clearer. Venus’ thicker atmosphere contains CO2, N2 and sulfuric chemicals as well as PH3, an indicator for the improbable life. Mercury’s atmosphere is rather poor, but is important partly because it can offer information of the planet’s formation. This article can help beginners obtain an understanding about two planets’ features in three aspects and aid students on similar topics. Overall, these results shed light on guiding further exploration of solar system.
Habitability
Mercury
Atmosphere of Venus
Planetary habitability
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