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Packing for Mars for kids
\"What is it like to float weightlessly in the air? What happens if you vomit in your helmet during a spacewalk? How do astronauts go to the bathroom? Is it true that they don't shower? Can farts really be deadly in space? Best-selling Mary Roach has the answers. In this whip-smart, funny, and informative young readers adaptation of her best-selling Packing for Mars, Roach guides us through the irresistibly strange, frequently gross, and awe-inspiring realm of space travel and life without gravity. From flying on NASA's Weightless Wonder to eating space food, Packing for Mars for Kids is chock-full of first-hand experiences and thorough research. Roach has crafted an authoritative and accessible book that is perfectly pitched to inquiring middle grade readers\"-- Provided by publisher.
Book
Dayside Transient Phenomena and Their Impact on the Magnetosphere and Ionosphere
Dayside transients, such as hot flow anomalies, foreshock bubbles, magnetosheath jets, flux transfer events, and surface waves, are frequently observed upstream from the bow shock, in the magnetosheath, and at the magnetopause. They play a significant role in the solar wind-magnetosphere-ionosphere coupling. Foreshock transient phenomena, associated with variations in the solar wind dynamic pressure, deform the magnetopause, and in turn generates field-aligned currents (FACs) connected to the auroral ionosphere. Solar wind dynamic pressure variations and transient phenomena at the dayside magnetopause drive magnetospheric ultra low frequency (ULF) waves, which can play an important role in the dynamics of Earth’s radiation belts. These transient phenomena and their geoeffects have been investigated using coordinated in-situ spacecraft observations, spacecraft-borne imagers, ground-based observations, and numerical simulations. Cluster, THEMIS, Geotail, and MMS multi-mission observations allow us to track the motion and time evolution of transient phenomena at different spatial and temporal scales in detail, whereas ground-based experiments can observe the ionospheric projections of transient magnetopause phenomena such as waves on the magnetopause driven by hot flow anomalies or flux transfer events produced by bursty reconnection across their full longitudinal and latitudinal extent. Magnetohydrodynamics (MHD), hybrid, and particle-in-cell (PIC) simulations are powerful tools to simulate the dayside transient phenomena. This paper provides a comprehensive review of the present understanding of dayside transient phenomena at Earth and other planets, their geoeffects, and outstanding questions.
Journal Article
The Power of Place : Rulers and Their Palaces, Landscapes, Cities, and Holy Places
\"The Power of Place explores the nature of power--the power of kings, emperors, and popes--through the places that these rulers created or developed, including palaces, cities, landscapes, holy places, inauguration sites, and burial places. Ranging across all of Europe from the first to the sixteenth centuries--from Prague and Seville to Palermo and the Oslo Fjord--David Rollason examines how these places conveyed messages of power and what those messages were. Rollason draws on the latest research in a range of disciplines--principally archaeology, and the histories of art, architecture, and landscape, as well as historical and literary studies--to investigate what the power of rulers consisted of. Was their power based on impersonal bureaucratic mechanisms, on personal relationships between rulers and subjects, or on strong beliefs in the quasi-divine status of rulers? How did impressive edifices support and emphasize these practices of power? Rollason takes readers to spectacular sites, including the remarkable remains of the tenth-century city of Madinat al-Zahra near Cordoba, the remarkably preserved palace-church of the emperor Charlemagne in Aachen, and the soaring shrine-church of the Saint-Chapelle of King Louis IX. Giving readers the tools to analyze rulers' palaces, landscapes, cities, and holy places, The Power of Place offers a fascinating perspective on the development of power throughout history\"-- Provided by publisher.
Book
Parker Solar Probe: Four Years of Discoveries at Solar Cycle Minimum
Launched on 12 Aug. 2018, NASA’s Parker Solar Probe had completed 13 of its scheduled 24 orbits around the Sun by Nov. 2022. The mission’s primary science goal is to determine the structure and dynamics of the Sun’s coronal magnetic field, understand how the solar corona and wind are heated and accelerated, and determine what processes accelerate energetic particles. Parker Solar Probe returned a treasure trove of science data that far exceeded quality, significance, and quantity expectations, leading to a significant number of discoveries reported in nearly 700 peer-reviewed publications. The first four years of the 7-year primary mission duration have been mostly during solar minimum conditions with few major solar events. Starting with orbit 8 (i.e., 28 Apr. 2021), Parker flew through the magnetically dominated corona, i.e., sub-Alfvénic solar wind, which is one of the mission’s primary objectives. In this paper, we present an overview of the scientific advances made mainly during the first four years of the Parker Solar Probe mission, which go well beyond the three science objectives that are: (1) Trace the flow of energy that heats and accelerates the solar corona and solar wind; (2) Determine the structure and dynamics of the plasma and magnetic fields at the sources of the solar wind; and (3) Explore mechanisms that accelerate and transport energetic particles.
Journal Article
Splash down!
\"Two lovable mismatched rovers are back for another adventure, this time on an oceanic planet! Organized, careful Rover and impulsive, excitable Speck are ready to set off on their next dangerous, hazardous, mysterious mission: a trip to Unexplored Planet K2-18b. Adventure is underway as they splash down onto the watery surface of this world and get to know the locals. Before long, the two rovers find themselves on a new mission: to help two Spikey-Spikes recover their missing brother from inside the belly of the terrifying Blubber Beast! Will Rover and Speck be able to outwit the Beast and save their new friend? Or will they get -- gulp -- swallowed up too? Jonathan Roth's hugely appealing graphic novel combines classic comic-style art with a gripping plot, loads of extra-silly laughs, and two endearing characters to root for. It's also a great introduction to real rovers and robots, and the entertaining science sidebars sprinkled throughout the story give readers a chance to learn about marine biology, ocean creatures, and more. Backmatter includes a drawing lesson ready-made for classrooms and a fun spot-the-differences activity. This winning combination of accessible STEM content, perfectly kid-friendly humor and loads of adventure is sure to satisfy armchair astronauts everywhere.\"--Provided by publisher
Book
Observation of inverse Compton emission from a long γ-ray burst
Long-duration γ-ray bursts (GRBs) originate from ultra-relativistic jets launched from
the collapsing cores of dying massive stars. They are characterized by an initial phase
of bright and highly variable radiation in the kiloelectronvolt-to-megaelectronvolt band, which is probably produced within the jet and lasts from milliseconds to minutes, known as the prompt emission. Subsequently, the interaction of the jet with the surrounding medium generates shock waves that are responsible for the afterglow emission, which lasts from days to months and occurs over a broad energy range from the radio to the gigaelectronvolt bands. The afterglow emission is generally well explained as synchrotron radiation emitted by electrons accelerated by the external shock. Recently, intense long-lasting emission between 0.2 and 1 teraelectronvolts was observed from GRB 190114C. Here we report multifrequency observations of GRB 190114C, and study the evolution in time of the GRB emission across 17 orders of magnitude in energy, from 5 × 10^(−6) to 10^(12) electronvolts. We find that the broadband spectral energy distribution is double-peaked, with the teraelectronvolt emission constituting a distinct spectral component with power comparable to the synchrotron component. This component is associated with the afterglow and is satisfactorily explained by inverse Compton up-scattering of synchrotron photons by high-energy electrons. We find that the conditions required to account for the observed teraelectronvolt component are typical for GRBs, supporting the possibility that inverse Compton emission is commonly produced in GRBs.
Journal Article
Tunable Laser Spectrometers for Planetary Science
Distinguishing planetary formation and evolution pathways and understanding the origins of volatiles on planetary bodies requires determination of relative abundances and isotope ratios in the noble gases, and also of the isotope ratios in C, H, N, O and S at high precisions. Traditional planetary mass spectrometers uniquely provide excellent survey capability including the noble gas relative abundances and their isotope ratios. However, to distinguish planetary evolution models for the outer planets, stable isotope ratios in C and O require precisions of ∼10 or better, readily achievable with a tunable laser spectrometer (TLS). As demonstrated on the Mars Curiosity rover, and as planned for a now-selected NASA Venus mission, tunable laser spectrometers play a unique role synergistic with the capabilities of planetary mass spectrometers. The TLS technique of recording infrared absorption spectra at ultrahigh resolution (resolving power λ/δλ ∼ 5 million) provides unambiguous detection of a wide variety of gases such as H2O, H2O2, H2CO, HOCl, NO, NO2, HNO3, N2O, O3, CO, CO2, NH3, N2H4, PH3, H2S, SO2, OCS, HCl, HF, O2, HCN, and CH4, C2H2, C2H4, C2H6 at parts-per-billion levels. Through line-depth or line-area ratio comparisons of adjacent spectral lines, planetary TLS instruments can achieve isotope ratio measurements in C, H, N, O, and S molecules at precisions of ∼1–2, including for the triple isotope components of O and S. Expected performance of TLS instruments for Venus, Saturn, Enceladus and Uranus will be described as constrained by actual measurements reported at Mars on the Curiosity rover.
Journal Article
Craters, boulders and regolith of (101955) Bennu indicative of an old and dynamic surface
Small, kilometre-sized near-Earth asteroids are expected to have young and frequently refreshed surfaces for two reasons: collisional disruptions are frequent in the main asteroid belt where they originate, and thermal or tidal processes act on them once they become near-Earth asteroids. Here we present early measurements of numerous large candidate impact craters on near-Earth asteroid (101955) Bennu by the OSIRIS-REx (Origins, Spectral Interpretation, Resource Identification, and Security-Regolith Explorer) mission, which indicate a surface that is between 100 million and 1 billion years old, predating Bennu’s expected duration as a near-Earth asteroid. We also observe many fractured boulders, the morphology of which suggests an influence of impact or thermal processes over a considerable amount of time since the boulders were exposed at the surface. However, the surface also shows signs of more recent mass movement: clusters of boulders at topographic lows, a deficiency of small craters and infill of large craters. The oldest features likely record events from Bennu’s time in the main asteroid belt.Near-Earth rubble-pile asteroid Bennu has an unexpectedly old surface, with numerous candidate impact craters and morphologically diverse boulders, according to early observations by the OSIRIS-REx mission.
Journal Article
The Mars Environmental Dynamics Analyzer, MEDA. A Suite of Environmental Sensors for the Mars 2020 Mission
NASA’s Mars 2020 (M2020) rover mission includes a suite of sensors to monitor current environmental conditions near the surface of Mars and to constrain bulk aerosol properties from changes in atmospheric radiation at the surface. The Mars Environmental Dynamics Analyzer (MEDA) consists of a set of meteorological sensors including wind sensor, a barometer, a relative humidity sensor, a set of 5 thermocouples to measure atmospheric temperature at ∼1.5 m and ∼0.5 m above the surface, a set of thermopiles to characterize the thermal IR brightness temperatures of the surface and the lower atmosphere. MEDA adds a radiation and dust sensor to monitor the optical atmospheric properties that can be used to infer bulk aerosol physical properties such as particle size distribution, non-sphericity, and concentration. The MEDA package and its scientific purpose are described in this document as well as how it responded to the calibration tests and how it helps prepare for the human exploration of Mars. A comparison is also presented to previous environmental monitoring payloads landed on Mars on the Viking, Pathfinder, Phoenix, MSL, and InSight spacecraft.
Journal Article
Defining the Middle Corona
The middle corona, the region roughly spanning heliocentric distances from 1.5 to 6 solar radii, encompasses almost all of the influential physical transitions and processes that govern the behavior of coronal outflow into the heliosphere. The solar wind, eruptions, and flows pass through the region, and they are shaped by it. Importantly, the region also modulates inflow from above that can drive dynamic changes at lower heights in the inner corona. Consequently, the middle corona is essential for comprehensively connecting the corona to the heliosphere and for developing corresponding global models. Nonetheless, because it is challenging to observe, the region has been poorly studied by both major solar remote-sensing and in-situ missions and instruments, extending back to the Solar and Heliospheric Observatory (SOHO) era. Thanks to recent advances in instrumentation, observational processing techniques, and a realization of the importance of the region, interest in the middle corona has increased. Although the region cannot be intrinsically separated from other regions of the solar atmosphere, there has emerged a need to define the region in terms of its location and extension in the solar atmosphere, its composition, the physical transitions that it covers, and the underlying physics believed to shape the region. This article aims to define the middle corona, its physical characteristics, and give an overview of the processes that occur there.
Journal Article