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  • 04. Solid Earth::04.06. Seismology::04.06.10. Instruments and techniques  (27)
  • 04. Solid Earth::04.08. Volcanology::04.08.01. Gases  (19)
  • Astronomy
  • J24
  • 2010-2014  (53)
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Years
Year
  • 1
    Publication Date: 2019-07-19
    Description: We present calculations of the early stages of the formation of Jupiter via core nucleated accretion and gas capture. The core begins as a seed body of about 350 kilometers in radius and orbits in a swarm of planetesimals whose initial radii range from 15 meters to 100 kilometers. We follow the evolution of the swarm by accounting for growth and fragmentation, viscous and gravitational stirring, and for drag-induced migration and velocity damping. Gas capture by the core substantially enhances the cross-section of the planet for accretion of small planetesimals. The dust opacity within the atmosphere surrounding the planetary core is computed self-consistently, accounting for coagulation and sedimentation of dust particles released in the envelope as passing planetesimals are ablated. The calculation is carried out at an orbital semi-major axis of 5.2 AU and an initial solids' surface density of 10/g/cm^2 at that distance. The results give a core mass of 7 Earth masses and an envelope mass of approximately 0.1 Earth mass after 500,000 years, at which point the envelope growth rate surpasses that of the core. The same calculation without the envelope gives a core mass of only 4 Earth masses.
    Keywords: Astronomy
    Type: ARC-E-DAA-TN10762 , NCTS# 16972-14; Annual Meeting, Division for Planetary Science; Oct 06, 2013 - Oct 11, 2013; Denver, CO; United States
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  • 2
    Publication Date: 2019-07-13
    Description: No abstract available
    Keywords: Astronomy
    Type: LWA Current and Future Users Meeting; May 12, 2011 - May 13, 2011; Albuquerque, NM; United States
    Format: text
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  • 3
    Publication Date: 2019-07-13
    Description: No abstract available
    Keywords: Astronomy
    Type: National Radio Science Meeting (USNC-URSI); Jan 05, 2011 - Jan 09, 2011; Boulder, CO; United States
    Format: text
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  • 4
    Publication Date: 2019-07-20
    Description: Disk disperse in a few million years, before which they must form planets. Photoevaporation and viscosity are mainly responsible for disk dispersal. EUV, FUV and X-rays have all been suggested as photoevaporation agents, disk evolutionary scenarios and predicted mass loss rates in each case differ. Stellar mass and radiation field, disk properties, magnitude of viscosity, and dust evolution all play significant roles in determining the evolution of the disk and its lifetime. Observational diagnostics of photoevaperative flows include [Nell] and perhaps [OI]. These are at present inconclusive and better diagnostics are needed.
    Keywords: Astronomy
    Type: ARC-E-DAA-TN17213 , The Disk in Relation to The Formation of Planets And Their Protoatmospheres; Aug 25, 2014 - Aug 29, 2014; Beijing; China
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  • 5
    Publication Date: 2019-07-13
    Description: Motivation for the study is: (1) Lunar Radio Array for low frequency, high redshift Dark Ages/Epoch of Reionization observations (z =6-50, f=30-200 MHz) (2) High precision cosmological measurements of 21 cm H I line fluctuations (3) Probe universe before first star formation and provide information about the Intergalactic Medium and evolution of large scale structures (5) Does the current cosmological model accurately describe the Universe before reionization? Lunar Radio Array is for (1) Radio interferometer based on the far side of the moon (1a) Necessary for precision measurements, (1b) Shielding from earth-based and solar RFI (12) No permanent ionosphere, (2) Minimum collecting area of approximately 1 square km and brightness sensitivity 10 mK (3)Several technologies must be developed before deployment The power needed to process signals from a large array of nonsteerable elements is not prohibitive, even for the Moon, and even in current technology. Two different concepts have been proposed: (1) Dark Ages Radio Interferometer (DALI) (2)( Lunar Array for Radio Cosmology (LARC)
    Keywords: Astronomy
    Type: National Radio Science Meeting; Jan 05, 2011; Boulder, CO; United States
    Format: text
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  • 6
    Publication Date: 2019-07-13
    Description: We report on multifrequency observations performed during 2012 December-2013 August of the first narrow-line Seyfert 1 galaxy detected in gamma rays, PMN J0948+0022 (z equal to 0.5846). A gamma-ray flare was observed by the Large Area Telescope on board Fermi during 2012 December-2013 January, reaching a daily peak flux in the 0.1-100 GeV energy range of (155 plus or minus 31)10(exp 8) ph cm (exp 2) s (exp 1) on 2013 January 1, corresponding to an apparent isotropic luminosity of approximately 1.510)exp 48) erg s(exp 1). The gamma-ray flaring period triggered Swift and VERITAS observations in addition to radio and optical monitoring by OVRO, MOJAVE, and CRTS. A strong flare was observed in optical, UV, and X- rays on 2012 December 30, quasi-simultaneously to the gamma-ray flare, reaching a record flux for this source from optical to gamma rays. VERITAS observations at very high energy (E greater than 100 GeV) during 2013 January 6-17 resulted in an upper limit of F(sub greater than 0.2 TeV) less than 4.0 10(exp 12) ph cm(exp 2) s(exp 1). We compared the spectral energy distribution (SED) of the flaring state in 2013 January with that of an intermediate state observed in 2011. The two SEDs, modelled as synchrotron emission and an external Compton scattering of seed photons from a dust torus, can be modelled by changing both the electron distribution parameters and the magnetic field.
    Keywords: Astronomy
    Type: GSFC-E-DAA-TN24339 , Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711) (e-ISSN 1365-2966); 446; 3; 2456-2467
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  • 7
    Publication Date: 2019-07-13
    Description: The architecture of a cross-correlator for a synthesis radio telescope with N greater than 1000 antennas is studied with the objective of minimizing power consumption. It is found that the optimum architecture minimizes memory operations, and this implies preference for a matrix structure over a pipeline structure and avoiding the use of memory banks as accumulation registers when sharing multiply-accumulators among baselines. A straw-man design for N = 2000 and bandwidth of 1 GHz, based on ASICs fabricated in a 90 nm CMOS process, is presented. The cross-correlator proper (excluding per-antenna processing) is estimated to consume less than 35 kW.
    Keywords: Astronomy
    Type: 2011 URSI General Assembly and Scientific Symposium; Aug 13, 2011 - Aug 20, 2011; Istanbul; Turkey
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  • 8
    Publication Date: 2017-04-04
    Description: It was the 2005 when management of the Centro Nazionale Terremoti, department of the Istituto Nazionale di Geofisica e Vulcanologia, thanks to funds of the Italian Civil Protection national service, decided to build its own first group of OBS’s. On July 2006, technicians of the Gibilmanna Observatory, seat of the “OBS Lab”, deployed the first prototype of OBS/H on the flat top of the Marsili submarine volcano. The nine days test, allow to record more than 1000 volcano-tectonic and regional events, among them, only nine were also recorded by the on-land seismic network, the others were related to the volcano activity. The successful test led to the construction of seven OBS’s equipped with: i) Nanometrics Trillium 120p seismic sensors (120s-175Hz), installed on a passive levelling system inside a 17” pressure glass sphere; ii) Cox-Webb Differential Pressure Gauge (500s – 2Hz) or HTI-04-PCA/ULF hydrophone (100s – 8kHz); iii) four channels, 21 bits, Send Geolon MLS digitizer. The ballast “burn-wire” release system is based on two different acoustic releasers, one backup of the other: i) Ixsea AR816S-MR, ii) Ore Offshore C980102. This solution, with two different releasers, installed in two different canisters, showed itself to be very reliable, allowing the recovery of the instrument also when one of the two releasers didn’t reply to the commands sent from the ship. At the end of the experiment, owing to the release of the ballast, the OBS’s come up to the surface thanks to the buoyancy of McLane and Vitrovex glass spheres and they are recovered with the help of Novatech radio beacons and xenon flashers. In case of unwished ballast release, a GPS based tracking system will supply, through a web platform, data for recovering of the instrument. This system allowed to recover one of the OBS’s deployed in the Aeolian islands area on July 2008: because of an electronic issue, the Ore Offshore releaser board gave voltage to the burn wire system and the instrument came up to the surface few hours after the deployment; the OBS was recovered three days after nearby the Straits of Messina. Trillium 120p seismometers, installed until the end of the 2008 on our OBS’s, have a very narrow operational tilt range: ±0.2°. Out of the range of ±0.1°, power consumption increases to 2.5W from the nominal 600mW. This high power consumption in the presence of tiny mechanical problems on the leveling system, leaded us to replace the Nanometrics sensors with Guralp CMG40T-OBS (60s – 100Hz), a low power sensor (about 150 mW) gimbaled and housed in a glass sphere with a diameter of 16 cm. First months of 2010 will see the birth of a new prototype of OBS. This new project provides the capability to communicate from the sea bottom to the surface: the instrument will be equipped with an embedded system, based on ARM processor, which will store and process seismic data coming from the seismometers and the DPG/hydrophone; a full depth acoustic modem will allow to transfer to the surface portion of seismic data (e. g. triggered earthquakes traces) or tsunami alarm. A new frame with syntactic foam instead of glass spheres was drawn to obtain the necessary buoyancy for the modem and its batteries pack.
    Description: Published
    Description: IPG, Paris
    Description: 2.5. Laboratorio per lo sviluppo di sistemi di rilevamento sottomarini
    Description: open
    Keywords: OBS ; OBS/H ; Ocean Bottom Seismometer ; 04. Solid Earth::04.06. Seismology::04.06.10. Instruments and techniques
    Repository Name: Istituto Nazionale di Geofisica e Vulcanologia (INGV)
    Type: Oral presentation
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  • 9
    Publication Date: 2017-04-04
    Description: The Ocean Bottom Seismometer with Hydrophone (OBS/H) is an autonomous data-acquisition system which free falls to the sea floor to record seismic and pressure signals generated by earthquakes and tsunamis. The development and the improvement of OBS/H's is a necessary process for seismological research institutions, because in the world about 90 percent of all natural earthquakes has epicenters in offshore areas. This paper describes the OBS/H developed by the “Istituto Nazionale di Geofisica e Vulcanologia” (INGV), designed to reliably collect broadband data from seafloor sites during long term deployment. The data recorded by seismometers on the sea floor is influenced by background noise. In particular, the free fall of the instrument and the subsequent dropping of the seismic sensor on the superficial sediments, could cause coupling problems with signals distortion and high level noise due to the sensor tilt. Supported by data acquired during several monitoring campaigns in the Mediterranean Sea, we will show that the INGV OBS/H is able to record high quality seismic signals with low noise levels and low distortion, proving a good coupling of the seismometer with the seabed.
    Description: Published
    Description: Santander, Spain
    Description: 2.5. Laboratorio per lo sviluppo di sistemi di rilevamento sottomarini
    Description: restricted
    Keywords: OBS/H ; OBS ; Ocean Bottom Seismometer ; Underwater monitoring ; 04. Solid Earth::04.06. Seismology::04.06.10. Instruments and techniques
    Repository Name: Istituto Nazionale di Geofisica e Vulcanologia (INGV)
    Type: Extended abstract
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  • 10
    Publication Date: 2017-04-04
    Description: No abstract
    Description: Published
    Description: 92-117
    Description: 4V. Vulcani e ambiente
    Description: restricted
    Keywords: geogenic gases ; gas hazard ; geomithology ; underworld ; 01. Atmosphere::01.01. Atmosphere::01.01.07. Volcanic effects ; 04. Solid Earth::04.04. Geology::04.04.12. Fluid Geochemistry ; 04. Solid Earth::04.08. Volcanology::04.08.01. Gases ; 04. Solid Earth::04.08. Volcanology::04.08.08. Volcanic risk
    Repository Name: Istituto Nazionale di Geofisica e Vulcanologia (INGV)
    Type: book chapter
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