Imprints of the Jittering Jets Explosion Mechanism in the Morphology of the Supernova Remnant SNR 0540-69.3     

Noam Soker 《天文和天体物理学研究(英文版)》2022,(3):186-193

I identify a point-symmetric structure in recently published VLT/MUSE velocity maps of different elements in a plane along the line of sight at the center of th...  相似文献   

Impact Assessment of Pumping Parameters on Groundwater Bacterial Communities     

Noam Shani  Vasantha Aravinthan  Pierre Rossi  Guillaume Laulan  Pascale Ducommun  Christof Holliger 《Ground Water Monitoring & Remediation》2013,33(2):31-37

Groundwater microbial community samples are traditionally collected using pumping techniques optimized for groundwater chemistry assessment, although the impact of groundwater pumping parameters on apparent bacterial community structures (BCSs) is not really known. We therefore studied the impact of pumping lift, flow regime, and tubing material on BCS, which were analyzed by terminal‐restriction fragment length polymorphism (T‐RFLP). Ruzicka dissimilarity coefficients were calculated between T‐RFLP profiles to assess disparities between BCS. Variations in pumping lift, flow regime, and tubing material did not affect the apparent BCS in experiments using a homogenous water system under laboratory conditions showing that the conditions within the tube had no detectable effect on BCS. However, pumping groundwater from aquifer monitoring wells at different flow rates in the field revealed a significant impact on the apparent BCS. Water samples collected from fine sediment were the most affected by the pumping flow rate.  相似文献   

Reply to comment by Ben-Zvi,A., D. Rosenfeld and A. Givati on the paper: Levin,Z., N. Halfon and P. Alpert, “Reassessment of rain experiments and operations in Israel including synoptic considerations,” Atmos. Res. 97, 513–525. DOI: 10.1016/j.atmosres.2010.06.011     

Zev Levin  Noam Halfon  Pinhas Alpert 《Atmospheric Research》2011,99(3-4):593-596

Levin et al. (2010; hereafter LHA) (Levin, Z., Halfon, N., Alpert, P., 2010. Reassessment of rain experiments and operations in Israel including synoptic considerations. Atmos. Res. 97, 513–525. DOI:10.1016/j.atmosres.2010.06.011.), reanalyzed the results of the operational seeding in northern Israel between 1975 and 2007 and the preceding Israel 2 cloud seeding experiment (1969–1975) and concluded that there is no net increase in precipitation over the target areas. Our analysis revealed that a synoptic bias during Israel 2 is one of the reasons for the apparent positive effect of seeding in the northern target area and the negative effect in the southern area both of which disappeared in the following experiment in the south (Israel 3; 1975–1995) and the operational seeding in the north.Ben-Zvi et al. (2010;hereafter BRG) criticized our paper primarily on the ground that we did not consider the positive results of Israel 1 experiment (1960–1967). It should be noted that in Israel 1 different seeding lines were used from those in both Israel 2 and the operational period. In addition, its raw data is not accessible anymore for reanalysis. Furthermore, Israel 2 had been designed as a confirmatory cross-over experiment to Israel 1 and failed to reproduce its promising results with double ratio (DR) of ~ 1.00, namely, zero rainfall enhancements. The same DR values were also found in Israel 3 and in the operational seeding. Therefore, because of the differences in the two experiments, the lack of access to the raw data and the disappointing results of the confirmatory experiment, we decided to concentrate our analysis on the more recent seeding activities.The attempt by BRG to explain the reduction of the DR to ~ 1.00 in the operational seeding period by the suppression due to pollution have been disproved by Alpert et al., 2008, Alpert et al., 2009 and also fail to explain the sharp decline of the target/control ratio right at the beginning of the operational seeding period when the lucky draw in this area came to its end (see LHA).  相似文献   

Spectral properties and geologic processes on Eros from combined NEAR NIS and MSI data sets     

Noam R. IZENBERG  Scott L. MURCHIE  James F. BELL  Lucy A. MCFADDEN  Dennis D. WELLNITZ  Beth E. CLARK  Michael J. GAFFEY 《Meteoritics & planetary science》2003,38(7):1053-1077

Abstract— From April 24 to May 14, 2000, the Near Earth Asteroid Rendezvous (NEAR) Shoemaker mission's near infrared spectrometer (NIS) obtained its highest resolution data of 433 Eros. High signal‐to‐noise ratio NIS reflectance spectra cover a wavelength range of 800–2400 nm, with footprint sizes from 213 times 427 m to 394 times 788 m. This paper describes improvement in instrument calibration by remediation of internally scattered light; derivation of a “pseudo channel” for NIS at 754 nm using Multispectral Imager (MSI) Eros approach maps at 951 and 754 nm; synthesis of a 3127‐spectrum high‐resolution data set with the improved calibration and expanded wavelength coverage; and investigation of global and localized spectral variation with respect to mineralogy, composition, and space weathering of Eros, comparing the findings with previous analyses. Scattered light removal reduces the “red” slope of Eros spectra, though not to the level seen by telescopic observations. The pseudo channel completes sampling of Eros' 1 micron (Band I) absorption feature, enabling direct comparison of NIS data with other asteroid and meteorite spectra without additional scaling or correction. Following scattered light removal and wavelength range extension, the spectral parameters of average Eros plot well inside the S(IV) field of Gaffey et al. (1993) and are consistent with the L6 chondrite meteorite fields of Gaffey and Gilbert (1998). Although Eros shows no evidence of mineralogical heterogeneity, modest spectral variations correlate with morphologically and geographically distinct areas of the asteroid. Eros bright‐to‐dark spectral ratios are largely consistent with laboratory “space weathering” experiment results and modeling of space weathering effects. Eros brightness variation unaccompanied by significant spectral variation departs from “lunar‐type”—where band depths, slopes, and albedoes all correlate—and “Ida‐type”—where significant spectral variation is unaccompanied by corresponding brightness variation. The brightest areas on Eros—steep crater walls—have lesser spectral slope and deeper Band I, consistent with exposure of “fresher,” less space weathered materials. Bright crater slope materials have opx/(opx + olv) of 0.24–0.29 and may be more representative of the subsurface mineralogy than “average” Eros, which is probably affected by space weathering. The floors of the large craters Psyche and Himeros have lower albedo and contain the most degraded or altered looking materials. NIS spectra retain a “red” spectral slope at greater than 2 microns. The recalibrated and expanded NIS spectra show better agreements with mixing models based on space weathering of chondritic mixtures.  相似文献   

Problems in suppressing cooling flows in clusters of galaxies by global heat conduction     

Noam Soker 《Monthly notices of the Royal Astronomical Society》2003,342(2):463-466

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Modelling the radio light curve of η Carinae     

Amit Kashi  Noam Soker 《Monthly notices of the Royal Astronomical Society》2007,378(4):1609-1618

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Satellite systems around galaxies in hydrodynamic simulations     

Noam I. Libeskind  Shaun Cole  Carlos S. Frenk  Takashi Okamoto  Adrian Jenkins 《Monthly notices of the Royal Astronomical Society》2007,374(1):16-28

We investigate the properties of satellite galaxies formed in N -body/SPH simulations of galaxy formation in the ΛCDM cosmology. The simulations include the main physical effects thought to be important in galaxy formation and, in several cases, produce realistic spiral discs. In total, a sample of nine galaxies of luminosity comparable to the Milky Way was obtained. At magnitudes brighter than the resolution limit,   M_V =−12  , the luminosity function of the satellite galaxies in the simulations is in excellent agreement with data for the Local Group. The radial number density profile of the model satellites, as well as their gas fractions also match observations very well. In agreement with previous N -body studies, we find that the satellites tend to be distributed in highly flattened configurations whose major axis is aligned with the major axis of the (generally triaxial) dark halo. In two out of three systems with sufficiently large satellite populations, the satellite system is nearly perpendicular to the plane of the galactic disc, a configuration analogous to that observed in the Milk Way. The discs themselves are perpendicular to the minor axis of their host haloes in the inner parts, and the correlation between the orientation of the galaxy and the shape of the halo persists even out to the virial radius. However, in one case the disc's minor axis ends up, at the virial radius, perpendicular to the minor axis of the halo. The angular momenta of the galaxies and their host halo tend to be well aligned.  相似文献   

Astrobiological molecularly imprinted polymer sensors     

Noam R. Izenberg 《Planetary and Space Science》2009,57(7):846-211

The purpose of the Astrobiological MIP Sensor (AMS) Project is to develop reliable, low-cost, low-mass, low-power consumption detection technologies for in situ analysis of biochemical markers, and other indicators of astrobiological importance. To this end, we are investigating the potential role that molecularly imprinted polymers (MIP) could serve in the recognition of pre-biotic and biotic compounds in planetary, astrobiological and geochemical mission profiles. While MIPs are effective molecular recognition tools, a signal transduction method must be developed so that the recognition of analytes can be realized. In the course of this study, surface plasmon resonance (SPR) will be the detection method of the MIP recognition event. In addition, MIP-coated SPR substrates were subjected to vibration, temperature and radiation testing to demonstrate that they could withstand the rigors of space travel. The methods developed in this study require capture of the biomarkers onto the SPR sensor chip, followed by addition of a MIP. It is the binding of the MIP to the SPR bound analyte that amplifies the SPR signal associated with binding of the low molecular weight analyte. The MIPs, developed in this study are water-soluble processable star polymers while the SPR device used was SensíQ™ by Nomatics. Proof-of-principal experiments were first demonstrated using amino biotin.  相似文献   

Explaining the energetic AGN outburst of MS 0735+7421 with massive slow jets     

Assaf Sternberg  Noam Soker 《Monthly notices of the Royal Astronomical Society》2009,398(1):422-428

By conducting axisymmetrical hydrodynamical numerical simulations (2.5 dimensional code) we show that slow, massive, wide jets can reproduce the morphology of the huge X-ray deficient bubble pair in the cluster of galaxies MS 0735+7421. The total energy of the jets, composed of the energy in the bubble pair and in the shock wave, is constrained by observations conducted by McNamara et al. to be  ∼10⁶² erg  . We show that two opposite jets that are active for ∼100 Myr, each with a launching half opening angle of  α≃ 70°  , an initial velocity of   v _j∼ 0.1 c   and a total mass loss rate of the two jets of     , can account for the observed morphology. Rapidly precessing narrow jets can be used instead of wide jets. In our model the cluster suffered from a cooling catastrophe ∼100 Myr ago. Most of the mass that cooled,  ∼10¹⁰ M_⊙  , was expelled back to the intracluster medium by the active galactic nuclei activity and is inside the bubbles now, ∼10 per cent formed stars and ∼10 per cent of the cold gas was accreted by the central black hole and was the source of the outburst energy. This type of activity is similar to that expected to occur in galaxy formation.  相似文献   

Prediction for the He iλ10830 Å absorption wing in the coming event of η Carinae     

Amit Kashi  Noam Soker 《Monthly notices of the Royal Astronomical Society》2009,394(2):923-928

We propose an explanation for the puzzling appearance of a wide blue absorption wing in the He  i  λ10830 Å  P Cygni profile of the massive binary star η Car several months before periastron passage. Our basic assumption is that the colliding winds region is responsible for the blue wing absorption. By fitting observations, we find that the maximum outflow velocity of this absorbing material is  ∼2300 km s⁻¹  . We also assume that the secondary star is towards the observer at periastron passage. With a toy model, we achieve two significant results. (1) We show that the semimajor axis orientation we use can account for the appearance and evolution of the wide blue wing under our basic assumption. (2) We predict that the Doppler shift (the edge of the absorption profile) will reach a maximum 0–3 weeks before periastron passage, and not necessarily exactly at periastron passage or after periastron passage.  相似文献