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Search Results: 1 - 10 of 403722 matches for " Sean M. Dougherty "
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Radio observations of colliding winds in massive stars
Sean M. Dougherty
Physics , 2009,
Abstract: This brief review describes radio observations of colliding winds in massive stars starting with the first direct observational support for the colliding-wind model advanced in the early 1990's to explain non-thermal radio and thermal X-ray emission in some massive stars. Studies of the well-studied and highly-eccentric WR+O star system WR140 are described along with recent observations of O-star systems. Also discussed is the binary nature of almost all massive stars that exhibit non-thermal behavior and some strategies for finding new systems.
Expanded Very Large Array
Sean M. Dougherty,Rick Perley
Physics , 2010,
Abstract: The Very Large Array is undergoing a major upgrade that will attain an order of magnitude improvement in continuum sensitivity across 1 to 50 GHz with instantaneous bandwidths up to 8 GHz in both polarizations. The new WIDAR correlator provides a highly flexible spectrometer with up to 16 GHz of bandwidth and a minimum of 16k channels for each array baseline. The new capabilities revolutionize the scientific discovery potential of the telescope. Early science programs are now underway. We provide an update on the status of the project and a description of early science programs.
WR146 - observing the OB-type companion
Sean M. Dougherty,P. M. Williams,D. L. Pollacco
Physics , 2000, DOI: 10.1046/j.1365-8711.2000.03504.x
Abstract: We present new radio and optical observations of the colliding-wind system WR146 aimed at understanding the nature of the companion to the Wolf-Rayet star and the collision of their winds. The radio observations reveal emission from three components: the WR stellar wind, the non-thermal wind-wind interaction region and, for the first time, the stellar wind of the OB companion. This provides the unique possibility of determining the mass-loss rate and terminal wind velocity ratios of the two winds, independent of distance. Respectively, these ratios are determined to be 0.20+/-0.06 and 0.56+/-0.17 for the OB-companion star relative to the WR star. A new optical spectrum indicates that the system is more luminous than had been believed previously. We deduce that the ``companion'' cannot be a single, low luminosity O8 star as previously suggested, but is either a high luminosity O8 star, or possibly an O8+WC binary system.
A radio-map of the colliding winds in the very massive binary system HD 93129A
Paula Benaglia,Benito Marcote,Javier Moldon,Ed Nelan,Michael De Becker,Sean M. Dougherty,Baerbel Koribalski
Physics , 2015, DOI: 10.1051/0004-6361/201425595
Abstract: Radio observations are an effective tool to discover particle acceleration regions in colliding-wind binaries, through detection of synchrotron radiation; these regions are natural laboratories for the study of relativistic particles. Wind-collision region (WCR) models can reproduce the radio continuum spectra of massive binaries that contain both thermal and non-thermal radio emission; however, key constraints for models come from high-resolution imaging. Only five WCRs have been resolved to date at radio frequencies at milliarcsec (mas) angular scales. The source HD 93129A, prototype of the very few known O2 I stars, is a promising target for study: recently, a second massive, early-type star about 50 mas away was discovered, and a non-thermal radio source detected in the region. Preliminary long-baseline array data suggest that a significant fraction of the radio emission from the system comes from a putative WCR. We sought evidence that HD 93129A is a massive binary system with colliding stellar winds that produce non-thermal radiation, through spatially resolved images of the radio emitting regions. We completed observations with the Australian Long Baseline Array (LBA) to resolve the system at mas angular resolutions and reduced archival Australia Telescope Compact Array (ATCA) data to derive the total radio emission. We also compiled optical astrometric data of the system in a homogeneous way. We reduced historical Hubble Space Telescope data and obtained absolute and relative astrometry with milliarcsec accuracy. The astrometric analysis leads us to conclude that the two stars in HD 93129A form a gravitationally bound system. The LBA data reveal an extended arc-shaped non-thermal source between the two stars, indicative of a WCR. The wind momentum-rate ratio of the two stellar winds is estimated. The ATCA data show a point source with a change in flux level ...
Growth Prospects in China and India Compared
Richard Herd,Sean Dougherty
The European Journal of Comparative Economics , 2007,
Abstract: This paper compares the growth prospects of China and India through a growth accounting analysis. Consistent time series for capital stock and employment are constructed using available survey data, and recent revisions to the national accounts for both countries are incorporated. The results allow for a discussion of the sources of growth in both countries, and a consideration of each country’s rate of potential growth in light of the outlook for national savings, as demographic shifts occur in each country
Comparing China and India: an Introduction
Sean Dougherty,Vittorio Valli
The European Journal of Comparative Economics , 2009,
Abstract: Editors' Introduction to the symposium "Comparing China and India: Structural Change and Development"
A Radio Pulsar Search of the Gamma-ray Binaries LS I +61 303 and LS 5039
M. Virginia McSwain,Paul S. Ray,Scott M. Ransom,Mallory S. E. Roberts,Sean M. Dougherty,Guy G. Pooley
Physics , 2011, DOI: 10.1088/0004-637X/738/1/105
Abstract: LS I +61 303 and LS 5039 are exceptionally rare examples of HMXBs with MeV-TeV emission, making them two of only five known or proposed "gamma-ray binaries". There has been disagreement within the literature over whether these systems are microquasars, with stellar winds accreting onto a compact object to produce high energy emission and relativistic jets, or whether their emission properties might be better explained by a relativistic pulsar wind colliding with the stellar wind. Here we present an attempt to detect radio pulsars in both systems with the Green Bank Telescope. The upper limits of flux density are between 4.1-14.5 uJy, and we discuss the null results of the search. Our spherically symmetric model of the wind of LS 5039 demonstrates that any pulsar emission will be strongly absorbed by the dense wind unless there is an evacuated region formed by a relativistic colliding wind shock. LS I +61 303 contains a rapidly rotating Be star whose wind is concentrated near the stellar equator. As long as the pulsar is not eclipsed by the circumstellar disk or viewed through the densest wind regions, detecting pulsed emission may be possible during part of the orbit.
Suzaku monitoring of the Wolf-Rayet binary WR140 around periastron passage: An approach for quantifying the wind parameters
Yasuharu Sugawara,Yoshitomo Maeda,Yohko Tsuboi,Kenji Hamaguchi,Michael Corcoran,A. M. T. Pollock,Anthony F. J. Moffat,Peredur M. Williams,Sean Dougherty,Julian Pittard
Physics , 2015, DOI: 10.1093/pasj/psv099
Abstract: Suzaku observations of the Wolf-Rayet binary WR 140 (WC7pd+O5.5fc) were made at four different times around periastron passage in 2009 January. The spectra changed in shape and flux with the phase. As periastron approached, the column density of the low-energy absorption increased, which indicates that the emission from the wind-wind collision plasma was absorbed by the dense W-R wind. The spectra can be mostly fitted with two different components: a warm component with kT=0.3--0.6 keV and a dominant hot component with kT~3 keV. The emission measure of the dominant, hot component is not inversely proportional to the distance between the two stars. This can be explained by the O star wind colliding before it has reached its terminal velocity, leading to a reduction in its wind momentum flux. At phases closer to periastron, we discovered a cool plasma component in a recombining phase, which is less absorbed. This component may be a relic of the wind-wind collision plasma, which was cooled down by radiation, and may represent a transitional stage in dust formation.
High resolution radio emission from RCW 49/Westerlund 2
Paula Benaglia,Baerbel Koribalski,Cintia S. Peri,Josep Marti,Juan R. Sanchez-Sutil,Sean M. Dougherty,Alberto Noriega-Crespo
Physics , 2013, DOI: 10.1051/0004-6361/201321976
Abstract: RCW49 and its ionizing cluster form an extensive, complex region, widely studied at IR and optical wavelengths. Molonglo 843 MHz and ATCA data at 1.4 and 2.4 GHz showed two shells. Recent high-resolution IR imaging revealed a complex dust structure and ongoing star formation. New high-bandwidth and high-resolution data of the RCW49 field were obtained to survey the radio emission at arcsec scale and investigate the small-scale features and nature of the HII region.- Data were collected with the new 2-GHz bandwidth receivers and the CABB correlator of the ATCA, at 5.5 and 9.0 GHz. In addition, archival observations at 1.4 and 2.4 GHz have been re-reduced and re-analyzed, together with optical, IR, X-ray, and gamma-ray observations.- The CABB data result in the most detailed radio continuum images of RCW49 to date. The radio emission closely mimics the near-IR emission observed by Spitzer, showing pillars and filaments. The brightest continuum emission comes from the region known as the bridge. The overall flattish spectral index is consistent with a free-free emission mechanism. However, hints of nonthermal components are also present in the bridge. A jet-like structure surrounded by a bubble feature whose nature is still unclear has been discovered close to the Westerlund~2 core. Two apparent bow shocks and a number of discrete sources have been detected as well in the surroundings of RCW49. We also report on and discuss the possible detection of a H RRL.- The radio results support an association between the cm continuum and molecular emission. The detection of the RRL kinematically favors a RCW49 distance of 6--7 kpc. If the negative spectral indices measured at the bridge are caused by synchrotron emission, we propose a scenario where high-energy emission could be produced. Finally, the newly discovered jet-like structure appears to deserve a detailed study by itself.
Induced Transcriptional Expression of Bacillus subtilis Amino Acid Permease yvbW in Response to Leucine Limitation  [PDF]
Sean M. Rollins
Advances in Microbiology (AiM) , 2014, DOI: 10.4236/aim.2014.48053

T box sequences have been identified upstream of a large number of uncharacterized genes such as transporters in bacterial genomes. Expression of each T box family gene is induced by limitation for a specific amino acid. T box family genes contain an untranslated leader region containing a factor-independent transcriptional terminator upstream of the structural genes. The anticodon of uncharged tRNA base-pairs with the leader mRNA at a codon referred to as the specifier sequence, inducing formation of an alternative antiterminator structure, allowing expression of the structural genes. There are several additional conserved primary sequence and secondary structural elements. Analysis of these elements can be used to predict the identity of the specifier codon and the amino acid signal. Bacillus subtilis hypothetical amino acid permease, yvbW, was analyzed as an example of this type of transcriptional regulatory prediction suggesting expression in response to leucine limitation. Expression was induced up to 130-fold in response to leucine limitation, utilizing a yvbW-lacZ transcriptional fusion. These data suggest that hypothetical amino acid permease YvbW may participate in leucine metabolism. A yvbW knockout strain was generated, although the substrate specificity for the putative amino acid permease was not identified.

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