ALBERT

Description: Author(s): M. A. Malkov, P. H. Diamond, and R. Z. Sagdeev The unexpected observation of an excess of positrons over electrons in cosmic ray experiments has generated a lot of excitement as a possible signature of dark matter. The authors of this recent Physical Review D paper suggest that astrophysical mechanisms involving ordinary matter could also account for the signal. The authors elucidate a new mechanism that would explain a significant part of the data. [Phys. Rev. D 94, 063006] Published Thu Sep 15, 2016

Description: Author(s): M. A. Malkov, P. H. Diamond, and R. Z. Sagdeev The much-anticipated proof of cosmic ray (CR) acceleration in supernova remnants must hinge on the full consistency of acceleration theory with the observations; direct proof is impossible because of CR-orbit scrambling. Recent observations indicate deviations between helium and proton CR rigidity s... [Phys. Rev. Lett. 108, 081104] Published Fri Feb 24, 2012

Description: 〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Sagdeev, R Z -- New York, N.Y. -- Science. 2001 Mar 2;291(5509):1663.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/11249808" target="_blank"〉PubMed〈/a〉

Description: An analytic solution describing an ion-acoustic collisionless shock, self-consistently with the evolution of shock-reflected ions, is obtained. The solution extends the classic soliton solution beyond a critical Mach number, where the soliton ceases to exist because of the upstream ion reflection. The reflection transforms the soliton into a shock with a trailing wave and a foot populated by the reflected ions. The solution relates parameters of the entire shock structure, such as the maximum and minimum of the potential in the trailing wave, the height of the foot, as well as the shock Mach number, to the number of reflected ions. This relation is resolvable for any given distribution of the upstream ions. In this paper, we have resolved it for a simple “box” distribution. Two separate models of electron interaction with the shock are considered. The first model corresponds to the standard Boltzmannian electron distribution in which case the critical shock Mach number only insignificantly increases from M ≈ 1.6 (no ion reflection) to M ≈ 1.8 (substantial reflection). The second model corresponds to adiabatically trapped electrons. They produce a stronger increase, from M ≈ 3.1 to M ≈ 4.5 . The shock foot that is supported by the reflected ions also accelerates them somewhat further. A self-similar foot expansion into the upstream medium is described analytically.

Description: Estimates can be made of unseen mass (in the form of cometary nuclei) at the heliocentric distances between 3 x 10(3) and 2 x 10(4) astronomical units(AU) under the assumptions (i) that the Oort cloud is a rarefied halo surrounding the core (dense, inner cometary cloud) and (ii) that the mass and albedo of comet Halley is typical for comets both in the core and the Oort cloud populations. The mass appears to be approximately 0.03 solar masses, with angular momentum of the order of 10(52) to 10(53) g-cm(2)/s. This mass is of the order of the total mass of the planetary system before the loss of volatiles. This leads to an estimate of a mass M(o) approximately 100 M( plus sign in circle) (where M( plus sign in circle) is the mass of Earth) concentrated in the Oort cloud (r 〉 2 x 10(4) AU) with an angular momentum that may exceed the present angular momentum of the whole planetary system by one order of magnitude. The present angular momentum of the Oort cloud appears to be of the same order as the total angular momentum of the planetary system before the loss of volatiles.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Marochnik, L S -- Mukhin, L M -- Sagdeev, R Z -- New York, N.Y. -- Science. 1988 Oct 28;242(4878):547-50.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17815893" target="_blank"〉PubMed〈/a〉

Description: 〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Gleick, P H -- Adams, R M -- Amasino, R M -- Anders, E -- Anderson, D J -- Anderson, W W -- Anselin, L E -- Arroyo, M K -- Asfaw, B -- Ayala, F J -- Bax, A -- Bebbington, A J -- Bell, G -- Bennett, M V L -- Bennetzen, J L -- Berenbaum, M R -- Berlin, O B -- Bjorkman, P J -- Blackburn, E -- Blamont, J E -- Botchan, M R -- Boyer, J S -- Boyle, E A -- Branton, D -- Briggs, S P -- Briggs, W R -- Brill, W J -- Britten, R J -- Broecker, W S -- Brown, J H -- Brown, P O -- Brunger, A T -- Cairns, J Jr -- Canfield, D E -- Carpenter, S R -- Carrington, J C -- Cashmore, A R -- Castilla, J C -- Cazenave, A -- Chapin, F S 3rd -- Ciechanover, A J -- Clapham, D E -- Clark, W C -- Clayton, R N -- Coe, M D -- Conwell, E M -- Cowling, E B -- Cowling, R M -- Cox, C S -- Croteau, R B -- Crothers, D M -- Crutzen, P J -- Daily, G C -- Dalrymple, G B -- Dangl, J L -- Darst, S A -- Davies, D R -- Davis, M B -- De Camilli, P V -- Dean, C -- DeFries, R S -- Deisenhofer, J -- Delmer, D P -- DeLong, E F -- DeRosier, D J -- Diener, T O -- Dirzo, R -- Dixon, J E -- Donoghue, M J -- Doolittle, R F -- Dunne, T -- Ehrlich, P R -- Eisenstadt, S N -- Eisner, T -- Emanuel, K A -- Englander, S W -- Ernst, W G -- Falkowski, P G -- Feher, G -- Ferejohn, J A -- Fersht, A -- Fischer, E H -- Fischer, R -- Flannery, K V -- Frank, J -- Frey, P A -- Fridovich, I -- Frieden, C -- Futuyma, D J -- Gardner, W R -- Garrett, C J R -- Gilbert, W -- Goldberg, R B -- Goodenough, W H -- Goodman, C S -- Goodman, M -- Greengard, P -- Hake, S -- Hammel, G -- Hanson, S -- Harrison, S C -- Hart, S R -- Hartl, D L -- Haselkorn, R -- Hawkes, K -- Hayes, J M -- Hille, B -- Hokfelt, T -- House, J S -- Hout, M -- Hunten, D M -- Izquierdo, I A -- Jagendorf, A T -- Janzen, D H -- Jeanloz, R -- Jencks, C S -- Jury, W A -- Kaback, H R -- Kailath, T -- Kay, P -- Kay, S A -- Kennedy, D -- Kerr, A -- Kessler, R C -- Khush, G S -- Kieffer, S W -- Kirch, P V -- Kirk, K -- Kivelson, M G -- Klinman, J P -- Klug, A -- Knopoff, L -- Kornberg, H -- Kutzbach, J E -- Lagarias, J C -- Lambeck, K -- Landy, A -- Langmuir, C H -- Larkins, B A -- Le Pichon, X T -- Lenski, R E -- Leopold, E B -- Levin, S A -- Levitt, M -- Likens, G E -- Lippincott-Schwartz, J -- Lorand, L -- Lovejoy, C O -- Lynch, M -- Mabogunje, A L -- Malone, T F -- Manabe, S -- Marcus, J -- Massey, D S -- McWilliams, J C -- Medina, E -- Melosh, H J -- Meltzer, D J -- Michener, C D -- Miles, E L -- Mooney, H A -- Moore, P B -- Morel, F M M -- Mosley-Thompson, E S -- Moss, B -- Munk, W H -- Myers, N -- Nair, G B -- Nathans, J -- Nester, E W -- Nicoll, R A -- Novick, R P -- O'Connell, J F -- Olsen, P E -- Opdyke, N D -- Oster, G F -- Ostrom, E -- Pace, N R -- Paine, R T -- Palmiter, R D -- Pedlosky, J -- Petsko, G A -- Pettengill, G H -- Philander, S G -- Piperno, D R -- Pollard, T D -- Price, P B Jr -- Reichard, P A -- Reskin, B F -- Ricklefs, R E -- Rivest, R L -- Roberts, J D -- Romney, A K -- Rossmann, M G -- Russell, D W -- Rutter, W J -- Sabloff, J A -- Sagdeev, R Z -- Sahlins, M D -- Salmond, A -- Sanes, J R -- Schekman, R -- Schellnhuber, J -- Schindler, D W -- Schmitt, J -- Schneider, S H -- Schramm, V L -- Sederoff, R R -- Shatz, C J -- Sherman, F -- Sidman, R L -- Sieh, K -- Simons, E L -- Singer, B H -- Singer, M F -- Skyrms, B -- Sleep, N H -- Smith, B D -- Snyder, S H -- Sokal, R R -- Spencer, C S -- Steitz, T A -- Strier, K B -- Sudhof, T C -- Taylor, S S -- Terborgh, J -- Thomas, D H -- Thompson, L G -- Tjian, R T -- Turner, M G -- Uyeda, S -- Valentine, J W -- Valentine, J S -- Van Etten, J L -- van Holde, K E -- Vaughan, M -- Verba, S -- von Hippel, P H -- Wake, D B -- Walker, A -- Walker, J E -- Watson, E B -- Watson, P J -- Weigel, D -- Wessler, S R -- West-Eberhard, M J -- White, T D -- Wilson, W J -- Wolfenden, R V -- Wood, J A -- Woodwell, G M -- Wright, H E Jr -- Wu, C -- Wunsch, C -- Zoback, M L -- Howard Hughes Medical Institute/ -- New York, N.Y. -- Science. 2010 May 7;328(5979):689-90. doi: 10.1126/science.328.5979.689.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20448167" target="_blank"〉PubMed〈/a〉

Description: The VEGA balloons made in situ measurements of pressure, temperature, vertical wind velocity, ambient light, frequency of lightning, and cloud particle backscatter. Both balloons encountered highly variable atmospheric conditions, with periods of intense vertical winds occurring sporadically throughout their flights. Downward winds as large as 3.5 meters per second occasionally forced the balloons to descend as much as 2.5 kilometers below their equilibrium float altitudes. Large variations, in pressure, temperature, ambient light level, and cloud particle backscatter (VEGA-1 only) correlated well during these excursions, indicating that these properties were strong functions of altitude in those parts of the middle cloud layer sampled by the balloons.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Sagdeev, R Z -- Linkin, V M -- Kerzhanovich, V V -- Lipatov, A N -- Shurupov, A A -- Blamont, J E -- Crisp, D -- Ingersoll, A P -- Elson, L S -- Preston, R A -- Hildebrand, C E -- Ragent, B -- Seiff, A -- Young, R E -- Petit, G -- Boloh, L -- Alexandrov, Y N -- Armand, N A -- Bakitko, R V -- Selivanov, A S -- New York, N.Y. -- Science. 1986 Mar 21;231(4744):1411-4.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17748081" target="_blank"〉PubMed〈/a〉

Description: A global array of 20 radio observatories was used to measure the three-dimensional position and velocity of the two meteorological balloons that were injected into the equatorial region of the Venus atmosphere near Venus midnight by the VEGA spacecraft on 11 and 15 June 1985. Initial analysis of only radial velocities indicates that each balloon was blown westward about 11,500 kilometers (8,000 kilometers on the night side) by zonal winds with a mean speed of about 70 meters per second. Excursions of the data from a model of constant zonal velocity were generally less than 3 meters per second; however, a much larger variation was evident near the end of the flight of the second balloon. Consistent systematic trends in the residuals for both balloons indicate the possibility of a solar-fixed atmospheric feature. Rapid variations in balloon velocity were often detected within a single transmission (330 seconds); however, they may represent not only atmospheric motions but also self-induced aerodynamic motions of the balloon.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Preston, R A -- Hildebrand, C E -- Purcell, G H Jr -- Ellis, J -- Stelzried, C T -- Finley, S G -- Sagdeev, R Z -- Linkin, V M -- Kerzhanovich, V V -- Altunin, V I -- Kogan, L R -- Kostenko, V I -- Matveenko, L I -- Pogrebenko, S V -- Strukov, I A -- Akim, E L -- Alexandrov, Y N -- Armand, N A -- Bakitko, R N -- Vyshlov, A S -- Bogomolov, A F -- Gorchankov, Y N -- Selivanov, A S -- Ivanov, N M -- Tichonov, V F -- Blamont, J E -- Boloh, L -- Laurans, G -- Boischot, A -- Biraud, F -- Ortega-Molina, A -- Rosolen, C -- Petit, G -- New York, N.Y. -- Science. 1986 Mar 21;231(4744):1414-6.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17748082" target="_blank"〉PubMed〈/a〉

Description: In June 1985, two instrumented balloons were placed in the atmosphere of Venus as part of the VEGA mission. Each balloon traveled about 30 percent of the way around the planet at a float altitude near 54 kilometers. In situ sensors measured pressure, temperature, vertical wind velocity, cloud particle backscatter, ambient light level, and frequency of lightning. A ground-based network of 20 radio antennas tracked the balloons by very long baseline interferometry (VLBI) techniques to monitor the Venus winds. The history, organization, and principal characteristics of this international balloon experiment are described.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Sagdeev, R Z -- Linkin, V M -- Blamont, J E -- Preston, R A -- New York, N.Y. -- Science. 1986 Mar 21;231(4744):1407-8.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17748079" target="_blank"〉PubMed〈/a〉