ALBERT

Beschreibung: Lunar true polar wander inferred from polar hydrogen Nature 531, 7595 (2016). doi:10.1038/nature17166 Authors: M. A. Siegler, R. S. Miller, J. T. Keane, M. Laneuville, D. A. Paige, I. Matsuyama, D. J. Lawrence, A. Crotts & M. J. Poston The earliest dynamic and thermal history of the Moon is not well understood. The hydrogen content of deposits near the lunar poles may yield insight into this history, because these deposits (which are probably composed of water ice) survive only if they remain in permanent shadow. If the orientation of the Moon has changed, then the locations of the shadowed regions will also have changed. The polar hydrogen deposits have been mapped by orbiting neutron spectrometers, and their observed spatial distribution does not match the expected distribution of water ice inferred from present-day lunar temperatures. This finding is in contrast to the distribution of volatiles observed in similar thermal environments at Mercury’s poles. Here we show that polar hydrogen preserves evidence that the spin axis of the Moon has shifted: the hydrogen deposits are antipodal and displaced equally from each pole along opposite longitudes. From the direction and magnitude of the inferred reorientation, and from analysis of the moments of inertia of the Moon, we hypothesize that this change in the spin axis, known as true polar wander, was caused by a low-density thermal anomaly beneath the Procellarum region. Radiogenic heating within this region resulted in the bulk of lunar mare volcanism and altered the density structure of the Moon, changing its moments of inertia. This resulted in true polar wander consistent with the observed remnant polar hydrogen. This thermal anomaly still exists and, in part, controls the current orientation of the Moon. The Procellarum region was most geologically active early in lunar history, which implies that polar wander initiated billions of years ago and that a large portion of the measured polar hydrogen is ancient, recording early delivery of water to the inner Solar System. Our hypothesis provides an explanation for the antipodal distribution of lunar polar hydrogen, and connects polar volatiles to the geologic and geophysical evolution of the Moon and the bombardment history of the early Solar System.

Beschreibung: When a massive star explodes as a supernova, substantial amounts of radioactive elements--primarily (56)Ni, (57)Ni and (44)Ti--are produced. After the initial flash of light from shock heating, the fading light emitted by the supernova is due to the decay of these elements. However, after decades, the energy powering a supernova remnant comes from the shock interaction between the ejecta and the surrounding medium. The transition to this phase has hitherto not been observed: supernovae occur too infrequently in the Milky Way to provide a young example, and extragalactic supernovae are generally too faint and too small. Here we report observations that show this transition in the supernova SN 1987A in the Large Magellanic Cloud. From 1994 to 2001, the ejecta faded owing to radioactive decay of (44)Ti as predicted. Then the flux started to increase, more than doubling by the end of 2009. We show that this increase is the result of heat deposited by X-rays produced as the ejecta interacts with the surrounding material. In time, the X-rays will penetrate farther into the ejecta, enabling us to analyse the structure and chemistry of the vanished star.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Larsson, J -- Fransson, C -- Ostlin, G -- Groningsson, P -- Jerkstrand, A -- Kozma, C -- Sollerman, J -- Challis, P -- Kirshner, R P -- Chevalier, R A -- Heng, K -- McCray, R -- Suntzeff, N B -- Bouchet, P -- Crotts, A -- Danziger, J -- Dwek, E -- France, K -- Garnavich, P M -- Lawrence, S S -- Leibundgut, B -- Lundqvist, P -- Panagia, N -- Pun, C S J -- Smith, N -- Sonneborn, G -- Wang, L -- Wheeler, J C -- England -- Nature. 2011 Jun 8;474(7352):484-6. doi: 10.1038/nature10090.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, The Oskar Klein Centre, Stockholm University, 106 91 Stockholm, Sweden. josefin.larsson@astro.su.se〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21654749" target="_blank"〉PubMed〈/a〉

Beschreibung: Observations with the Hubble Space Telescope (HST), conducted since 1990, now offer an unprecedented glimpse into fast astrophysical shocks in the young remnant of supernova 1987A. Comparing observations taken in 2010 with the use of the refurbished instruments on HST with data taken in 2004, just before the Space Telescope Imaging Spectrograph failed, we find that the Lyalpha and Halpha lines from shock emission continue to brighten, whereas their maximum velocities continue to decrease. We observe broad, blueshifted Lyalpha, which we attribute to resonant scattering of photons emitted from hot spots on the equatorial ring. We also detect N v lambdalambda1239, 1243 angstrom line emission, but only to the red of Lyalpha. The profiles of the N v lines differ markedly from that of Halpha, suggesting that the N4+ ions are scattered and accelerated by turbulent electromagnetic fields that isotropize the ions in the collisionless shock.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉France, Kevin -- McCray, Richard -- Heng, Kevin -- Kirshner, Robert P -- Challis, Peter -- Bouchet, Patrice -- Crotts, Arlin -- Dwek, Eli -- Fransson, Claes -- Garnavich, Peter M -- Larsson, Josefin -- Lawrence, Stephen S -- Lundqvist, Peter -- Panagia, Nino -- Pun, Chun S J -- Smith, Nathan -- Sollerman, Jesper -- Sonneborn, George -- Stocke, John T -- Wang, Lifan -- Wheeler, J Craig -- New York, N.Y. -- Science. 2010 Sep 24;329(5999):1624-7. doi: 10.1126/science.1192134. Epub 2010 Sep 2.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309-0389, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20813921" target="_blank"〉PubMed〈/a〉

Beschreibung: The earliest dynamic and thermal history of the Moon is not well understood. The hydrogen content of deposits near the lunar poles may yield insight into this history, because these deposits (which are probably composed of water ice) survive only if they remain in permanent shadow. If the orientation of the Moon has changed, then the locations of the shadowed regions will also have changed. The polar hydrogen deposits have been mapped by orbiting neutron spectrometers, and their observed spatial distribution does not match the expected distribution of water ice inferred from present-day lunar temperatures. This finding is in contrast to the distribution of volatiles observed in similar thermal environments at Mercury's poles. Here we show that polar hydrogen preserves evidence that the spin axis of the Moon has shifted: the hydrogen deposits are antipodal and displaced equally from each pole along opposite longitudes. From the direction and magnitude of the inferred reorientation, and from analysis of the moments of inertia of the Moon, we hypothesize that this change in the spin axis, known as true polar wander, was caused by a low-density thermal anomaly beneath the Procellarum region. Radiogenic heating within this region resulted in the bulk of lunar mare volcanism and altered the density structure of the Moon, changing its moments of inertia. This resulted in true polar wander consistent with the observed remnant polar hydrogen. This thermal anomaly still exists and, in part, controls the current orientation of the Moon. The Procellarum region was most geologically active early in lunar history, which implies that polar wander initiated billions of years ago and that a large portion of the measured polar hydrogen is ancient, recording early delivery of water to the inner Solar System. Our hypothesis provides an explanation for the antipodal distribution of lunar polar hydrogen, and connects polar volatiles to the geologic and geophysical evolution of the Moon and the bombardment history of the early Solar System.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Siegler, M A -- Miller, R S -- Keane, J T -- Laneuville, M -- Paige, D A -- Matsuyama, I -- Lawrence, D J -- Crotts, A -- Poston, M J -- England -- Nature. 2016 Mar 24;531(7595):480-4. doi: 10.1038/nature17166.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Planetary Science Institute, Tucson, Arizona 85719, USA. ; Southern Methodist University, Dallas, Texas 75275, USA. ; University of Alabama in Huntsville, Huntsville, Alabama 35899, USA. ; Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona 85721, USA. ; Earth Life Sciences Institute, Tokyo Institute of Technology, Meguro, Tokyo 152-8551, Japan. ; University of California, Los Angeles, California 90095, USA. ; The Johns Hopkins University Applied Physics Laboratory, Laurel, Maryland 20723, USA. ; Columbia University, New York, New York 10027, USA. ; California Institute of Technology, Pasadena, California 91125, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/27008966" target="_blank"〉PubMed〈/a〉