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• Journal article
  Zhong J, Pu ZY, Dunlop MW, Bogdanova YV, Wang XG, Xiao CJ, Guo RL, Hasegawa H, Raeder J, Zhou XZ, Angelopoulos V, Zong QG, Fu SY, Xie L, Taylor MGGT, Shen C, Berchem J, Zhang QH, Volwerk M, Eastwood JPet al., 2013,
  , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 118, Pages: 1904-1911, ISSN: 2169-9380
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  • Citations: 46
• Journal article
  Bowman KW, Shindell DT, Worden HM, Lamarque JF, Young PJ, Stevenson DS, Qu Z, de la Torre M, Bergmann D, Cameron-Smith PJ, Collins WJ, Doherty R, Dalsøren SB, Faluvegi G, Folberth G, Horowitz LW, Josse BM, Lee YH, MacKenzie IA, Myhre G, Nagashima T, Naik V, Plummer DA, Rumbold ST, Skeie RB, Strode SA, Sudo K, Szopa S, Voulgarakis A, Zeng G, Kulawik SS, Aghedo AM, Worden JRet al., 2013,
  , Atmospheric Chemistry and Physics, Vol: 13, Pages: 4057-4072
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• Journal article
  Simon S, van Treeck SC, Wennmacher A, Saur J, Neubauer FM, Bertucci CL, Dougherty MKet al., 2013,
  , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 118, Pages: 1679-1699, ISSN: 2169-9380
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  • Citations: 34
• Journal article
  Sergis N, Jackman CM, Masters A, Krimigis SM, Thomsen MF, Hamilton DC, Mitchell DG, Dougherty MK, Coates AJet al., 2013,
  , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 118, Pages: 1620-1634, ISSN: 2169-9380
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  • Citations: 38
• Journal article
  Messori G, Czaja A, 2013,
  , QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY, Vol: 139, Pages: 999-1008, ISSN: 0035-9009
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  • Citations: 26
• Journal article
  Hellinger P, Trávníček PM, Štverák Š, Matteini L, Velli Met al., 2013,
  , Journal of Geophysical 91��ɫ: Space Physics, Vol: 118, Pages: 1351-1365, ISSN: 2169-9380

  <jats:p>The proton thermal energetics in the slow solar wind between 0.3 and 1 AU is reinvestigated using the Helios 1 and 2 data, complementing a similar analysis for the fast solar wind [Hellinger et al., 2011]. The results for slow and fast solar winds are compared and discussed in the context of previous results. Protons need to be heated in the perpendicular direction with respect to the ambient magnetic field from 0.3 to 1 AU. In the parallel direction, protons need to be cooled at 0.3 AU, with a cooling rate comparable to the corresponding perpendicular heating rate; between 0.3 and 1 AU, the required cooling rate decreases until a transition to heating occurs: by 1 AU the protons require parallel heating, with a heating rate comparable to that required to sustain the perpendicular temperature. The heating/cooling rates (per unit volume) in the fast and slow solar winds are proportional to the ratio between the proton kinetic energy and the expansion time. On average, the protons need to be heated and the necessary heating rates are comparable to the energy cascade rate of the magnetohydrodynamic turbulence estimated from the stationary Kolmogorov‐Yaglom law at 1 AU; however, in the expanding solar wind, the stationarity assumption for this law is questionable. The turbulent energy cascade may explain the average proton energetics (although the stationarity assumption needs to be justified) but the parallel cooling is likely related to microinstabilities connected with the structure of the proton velocity distribution function. This is supported by linear analysis based on observed data and by results of numerical simulations.</jats:p>

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• Journal article
  Grasset O, Dougherty MK, Coustenis A, Bunce EJ, Erd C, Titov D, Blanc M, Coates A, Drossart P, Fletcher LN, Hussmann H, Jaumann R, Krupp N, Lebreton J-P, Prieto-Ballesteros O, Tortora P, Tosi F, Van Hoolst Tet al., 2013,
  , PLANETARY AND SPACE SCIENCE, Vol: 78, Pages: 1-21, ISSN: 0032-0633
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  • Citations: 548
• Journal article
  Zhong W, Haigh JD, 2013,
  , WEATHER, Vol: 68, Pages: 100-105, ISSN: 0043-1656
  • Cite
  • Citations: 58
• Journal article
  Badman SV, Masters A, Hasegawa H, Fujimoto M, Radioti A, Grodent D, Sergis N, Dougherty MK, Coates AJet al., 2013,
  , GEOPHYSICAL RESEARCH LETTERS, Vol: 40, Pages: 1027-1031, ISSN: 0094-8276
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  • Citations: 73
• Journal article
  Coustenis A, Atreya S, Castillo J, Coll P, Mueller-Wodarg I, Spilker Let al., 2013,
  , PLANETARY AND SPACE SCIENCE, Vol: 77, Pages: 1-2, ISSN: 0032-0633
  • Cite
  • Citations: 1
• Journal article
  Vigren E, Galand M, Yelle RV, Cui J, Wahlund J-E, Agren K, Lavvas PP, Mueller-Wodarg ICF, Strobel DF, Vuitton V, Bazin Aet al., 2013,
  , ICARUS, Vol: 223, Pages: 234-251, ISSN: 0019-1035
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  • Citations: 36
• Journal article
  Masters A, Stawarz L, Fujimoto M, Schwartz SJ, Sergis N, Thomsen MF, Retino A, Hasegawa H, Zieger B, Lewis GR, Coates AJ, Canu P, Dougherty MKet al., 2013,
  , NATURE PHYSICS, Vol: 9, Pages: 164-167, ISSN: 1745-2473
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  • Citations: 77
• Journal article
  Lavvas P, Yelle RV, Koskinen T, Bazin A, Vuitton V, Vigren E, Galand M, Wellbrock A, Coates AJ, Wahlund J-E, Crary FJ, Snowden Det al., 2013,
  , PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA, Vol: 110, Pages: 2729-2734, ISSN: 0027-8424
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  • Citations: 122
• Journal article
  Matteini L, Landi S, Velli M, Matthaeus WHet al., 2013,
  , The Astrophysical Journal: an international review of astronomy and astronomical physics, Vol: 763, ISSN: 0004-637X

  We investigate the role of kinetic instabilities driven by a proton anisotropy on the onset of magnetic reconnection by means of two-dimensional hybrid simulations. The collisionless tearing of a current sheet is studied in the presence of a proton temperature anisotropy in the surrounding plasma. Our results confirm that anisotropic protons within the current sheet region can significantly enhance/stabilize the tearing instability of the current. Moreover, fluctuations associated with linear instabilities excited by large proton temperature anisotropies can significantly influence the stability of the plasma and perturb the current sheets, triggering the tearing instability. We find that such a complex coupling leads to a faster tearing evolution in the $T_\perp >T_\Vert$ regime when an ion-cyclotron instability is generated by the anisotropic proton distribution functions. On the contrary, in the presence of the opposite anisotropy, fire-hose fluctuations excited by the unstable background protons with $T_\Vert <T_\perp$ are not able to efficiently destabilize current sheets, which remain stable for a long time after fire-hose saturation. We discuss possible influences of this novel coupling on the solar wind and heliospheric plasma dynamics.

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• Journal article
  Shi QQ, Zong Q-G, Fu SY, Dunlop MW, Pu ZY, Parks GK, Wei Y, Li WH, Zhang H, Nowada M, Wang YB, Sun WJ, Xiao T, Reme H, Carr C, Fazakerley AN, Lucek Eet al., 2013,
  , NATURE COMMUNICATIONS, Vol: 4, ISSN: 2041-1723
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  • Citations: 81
• Journal article
  Cargill P, 2013,
  , NATURE, Vol: 493, Pages: 485-486, ISSN: 0028-0836
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  • Citations: 10
• Journal article
  Cui J, Lian Y, Mueller-Wodarg ICF, 2013,
  , GEOPHYSICAL RESEARCH LETTERS, Vol: 40, Pages: 43-47, ISSN: 0094-8276
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  • Citations: 17
• Journal article
  Wicks RT, Mallet A, Horbury TS, Chen CHK, Schekochihin AA, Mitchell JJet al., 2013,
  , Physical Review Letters, Vol: 110, Pages: 025003-025003, ISSN: 0031-9007
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• Conference paper
  Fox C, Pickering JC, Beeby R, Murray JE, Last A, Green PDet al., 2013,

  Studies of the far IR water vapour continuum from CAVIAR and RHUBC campaigns using TAFTS

  We report results from the participation of the 91��ɫ College TAFTS instrument in the CAVIAR and RHUBC field campaigns, validating a derived water vapor continuum parameterization in the far-IR spectral region. © OSA 2013.

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• Conference paper
  Fox C, Pickering JC, Beeby R, Murray JE, Last A, Green PDet al., 2013,

  Studies of the far IR water vapour continuum from caviar and RHUBC campaigns using TAFTS

  We report results from the participation of the 91��ɫ College TAFTS instrument in the CAVIAR and RHUBC field campaigns, validating a derived water vapor continuum parameterization in the far-IR spectral region. © OSA 2013.

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• Conference paper
  Fox C, Pickering JC, Beeby R, Murray JE, Last A, Green PDet al., 2013,

  We report results from the participation of the 91��ɫ College TAFTS instrument in the CAVIAR and RHUBC field campaigns, validating a derived water vapor continuum parameterization in the far-IR spectral region. © OSA 2013.

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• Conference paper
  Fox C, Pickering JC, Beeby R, Murray JE, Last A, Green PDet al., 2013,

  Studies of the far IR water vapour continuum from caviar and RHUBC campaigns using TAFTS

  We report results from the participation of the 91��ɫ College TAFTS instrument in the CAVIAR and RHUBC field campaigns, validating a derived water vapor continuum parameterization in the far-IR spectral region. © OSA 2013.

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• Conference paper
  Seo Y, Chae KS, Mochizuki B, Clarino D, Yeung N, Yoon S, Seon J, Jin H, Lee DH, Lin RP, Sample J, Immel T, Brown P, Horbury TSet al., 2013,

  Instrument interface module between the on-board-computer and payloads in cinema CUBESAT as developed with FPGA

  , Pages: 4275-4281, ISSN: 0074-1795

  TRiplet Ionospheric Observatory-Cubesat for Ion, Neutral, Electron and MAgnetic fields (TRIO-CINEMA) is a space science mission consisting of three identical 3U CubeSats to provide stereo Energetic Neutral Atom (ENA) imaging of the ring current, multi-point in-situ measurement of supra thermal electrons and ions, and measurement of magnetic fields in Low Earth Orbit (LEO). Each spacecraft is equipped with a Supra Thermal Electrons, Ions, Neutrals (STEIN) instrument and a MAGnetometer from 91��ɫ College (MAGIC) instrument in order to measure the plasma particles with diverse species and energies and magnetic fields. STEIN is able to distinguish electrons, ions, and neutrals by applying electric field in the entrance aperture. MAGIC is a dual 3-axis magnetoresistive sensor intended for attitude control and scientific measurement. The standard spacecraft CubeSat employed for the TRIO- CINEMA mission often utilizes Commercial-Off-The Shelf (COTS) electronics to build bus avionics that provides power and communications, whereas payloads are usually built in accordance with specific requirements that are often more demanding in terms of generation, transmission and storage of the data and power consumption. Therefore, designing and developing the interface to be compatible between mission payloads and the CubeSat avionics built with COTS will be required for many CubeSat missions. In this presentation, we describe the instrument interface module between the On-Board-Computer (OBC) and the mission payloads for TRIO-CINEMA spacecraft. The module is developed to provide required communication and power interfaces. In the instrument interface module, a Field Programmable Gate Array (FPGA) is employed to support computing power of the OBC and communication interfaces. It is exclusively operated as data buffer and framer for generated data from mission payloads and their subsequent transmission through S-band to the ground station. The interface module provides various elect

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• Conference paper
  Masters A, Stawarz Ł, Fujimoto M, Schwartz SJ, Sergis N, Thomsen MF, Retinò A, Hasegawa H, Zieger B, Lewis GR, Coates AJ, Canu P, Dougherty MKet al., 2013,

  Electron acceleration to relativistic energies at a strong quasi-parallel shock wave

  Electrons can be accelerated to ultrarelativistic energies at strong (high-Mach number) collisionless shock waves that form when stellar debris rapidly expands after a supernova [4, 2, 19]. Collisionless shock waves also form in the flow of particles from the Sun (the solar wind), and extensive spacecraft observations have established that electron acceleration at these shocks is effectively absent whenever the upstream magnetic field is roughly parallel to the shock surface normal (quasi-parallel conditions) [16, 8, 10, 17, 14]. However, it is unclear whether this magnetic dependence of electron acceleration also applies to the far stronger shocks around young supernova remnants, where local magnetic conditions are poorly understood. Here we present Cassini spacecraft observations of an unusually strong solar system shock wave (Saturn’s bow shock) where significant local electron acceleration has been confirmed under quasi- parallel magnetic conditions for the first time, contradicting the established magnetic dependence of electron acceleration at solar system shocks [16, 8, 10, 17, 14]. Furthermore, the acceleration led to electrons at relativistic energies (∼ MeV), comparable to the highest energies ever attributed to shock-acceleration in the solar wind [16]. These observations suggest that at high-Mach numbers, like those of young supernova remnant shocks, quasi-parallel shocks become considerably more effective electron accelerators. For full details please see: Nature Physics, Volume 9, Issue 3, pp. 164-167.

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• Journal article
  Nakamura R, Plaschke F, Teubenbacher R, Giner L, Baumjohann W, Magnes W, Steller M, Torbert RB, Vaith H, Chutter M, Fornacon K-H, Glassmeier K-H, Carr Cet al., 2013,
  , GEOSCIENTIFIC INSTRUMENTATION METHODS AND DATA SYSTEMS, Vol: 3, Pages: 459-487, ISSN: 2193-0856
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• Journal article
  Pudney MA, Carr CM, Schwartz SJ, Howarth SIet al., 2013,
  , GEOSCIENTIFIC INSTRUMENTATION METHODS AND DATA SYSTEMS, Vol: 3, Pages: 437-458, ISSN: 2193-0856
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• Journal article
  Kasahara S, Kronberg EA, Kimura T, Tao C, Badman SV, Masters A, Retino A, Krupp N, Fujimoto Met al., 2013,
  , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 118, Pages: 375-384, ISSN: 2169-9380
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  • Citations: 49
• Journal article
  Banks JR, Brindley HE, 2013,
  , REMOTE SENSING OF ENVIRONMENT, Vol: 128, Pages: 58-73, ISSN: 0034-4257
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  • Citations: 57
• Journal article
  Orr A, Bracegirdle TJ, Hosking JS, Feng W, Roscoe HK, Haigh JDet al., 2013,
  , JOURNAL OF CLIMATE, Vol: 26, Pages: 662-668, ISSN: 0894-8755
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  • Citations: 16
• Journal article
  Graven HD, Xu X, Guilderson TP, Keeling RF, Trumbore SE, Tyler Set al., 2013,
  , RADIOCARBON, Vol: 55, Pages: 1541-1545, ISSN: 0033-8222
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  • Citations: 8

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