42,042 research outputs found
A 2 h periodic variation in the low-mass X-ray binary Ser X-1
No full textSpectroscopy of the low-mass X-ray binary Ser X-1 using the Gran Telescopio Canarias have revealed a ?2 h periodic variability that is present in the three strongest emission lines. We tentatively interpret this variability as due to orbital motion, making it the first indication of the orbital period of Ser X-1. Together with the fact that the emission lines are remarkably narrow, but still resolved, we show that a main-sequence K dwarf together with a canonical 1.4 M? neutron star gives a good description of the system. In this scenario, the most likely place for the emission lines to arise is the accretion disc, instead of a localized region in the binary (such as the irradiated surface or the stream-impact point), and their narrowness is due instead to the low inclination (?10°) of Ser X-1
The long-wavelength view of GG Tau A: rocks in the ring world
No full textWe present the first detection of GG Tau A at centimetre wavelengths, made with the Arcminute Microkelvin Imager Large Array at a frequency of 16 GHz (λ = 1.8 cm). The source is detected at >6 σrms with an integrated flux density of S16GHz = 249 ± 45 µJy. We use these new centimetre-wave data, in conjunction with additional measurements compiled from the literature, to investigate the long-wavelength tail of the dust emission from this unusual protoplanetary system. We use an MCMC-based method to determine maximum likelihood parameters for a simple parametric spectral model and consider the opacity and mass of the dust contributing to the microwave emission. We derive a dust mass of Md ~ 0.1 Msun, constrain the dimensions of the emitting region and find that the opacity index at λ > 7 mm is less than unity, implying a contribution to the dust population from grains exceeding ~4 cm in size. We suggest that this indicates coagulation within the GG Tau A system has proceeded to the point where dust grains have grown to the size of small rocks with dimensions of a few centimetres. Considering the relatively young age of the GG Tau association in combination with the low derived disc mass, we suggest that this system may provide a useful test case for rapid core accretion planet formation models
Iolaus nursei Butler 1896
No full textIolaus nursei Butler Aqabet Al-Baha-Tihama 20.00000° N, 41.43758°E: March 2012.Published as part of El-Hawagry, Magdi S., Sharaf, Mostafa R., Al Dhafer, Hathal M., Fadl, Hassan H. & Aldawood, Abdulrahman S., 2015, Addenda to the insect fauna of Al-Baha Province, Kingdom of Saudi Arabia with zoogeographical notes, pp. 1209-1236 in Journal of Natural History 50 on page 1221, DOI: 10.1080/00222933.2015.1103913, http://zenodo.org/record/399024
Precision nanomedicines for prostate cancer
No full textEditorial. Published online: 27 February 2018Anna Cifuentes-Rius, Lisa M Butler and Nicolas H Voelcke
Measurement of the D*(2010) branching fractions
No full textcomplete author list:
Butler F.; Fu X.; Kalbfleisch G.; Lambrecht M.; Ross W.; Skubic P.; Snow J.; Wang P.; Bortoletto D.; Brown D.; Dominick J.; Mcilwain R.; Miao T.; Miller D.; Modesitt M.; Schaffner S.; Shibata E.; Shipsey I.; Battle M.; Ernst J.; Kroha H.; Roberts S.; Sparks K.; Thorndike E.; Wang C.; Sanghera S.; Skwarnicki T.; Stroynowski R.; Artuso M.; Goldberg M.; Horwitz N.; Kennett R.; Moneti G.; Muheim F.; Playfer S.; Rozen Y.; Rubin P.; Stone S.; Thulasidas M.; Yao W.; Zhu G.; Barnes A.; Bartelt J.; Csorna S.; Egyed Z.; Jain V.; Sheldon P.; Akerib D.; Barish B.; Chadha M.; Cowen D.; Eigen G.; Miller J.; Urheim J.; Weinstein A.; Bean A.; Gronberg J.; Kutschke R.; Weinstein A.; Menary S.; Morrison R.; Nelson H.; Richman J.; Tajima H.; Schmidt D.; Sperka D.; Witherell M.; Acosta D.; Masek G.; Ong B.; Paar H.; Sivertz M.; Procario M.; Daoudi M.; Ford W.; Johnson D.; Lingel K.; Lohner M.; Rankin P.; Smith J.; Alexander J.; Bebek C.; Berkelman K.; Besson D.; Browder T.; Cassel D.; Coffman D.; Drell P.; Ehrlich R.; Galik R.; Garcia-Sciveres M.; Geiser B.; Gittleman B.; Gray S.; Hartill D.; Heltsley B.; Honscheid K.; Jones C.; Kandaswamy J.; Katayama N.; Kim P.; Kreinick D.; Ludwig G.; Masui J.; Mevissen J.; Mistry N.; Ng C.; Nordberg E.; O'Grady C.; Patterson J.; Peterson D.; Riley D.; Sapper M.; Selen M.; Worden H.; Worris M.; Würthwein F.; Avery P.; Freyberger A.; Rodriguez J.; Stephens R.; Yelton J.; Cinabro D.; Henderson S.; Kinoshita K.; Liu T.; Saulnier M.; Wilson R.; Yamamoto H.; Sadoff A.; Ammar R.; Ball S.; Baringer P.; Coppage D.; Copty N.; Davis R.; Hancock N.; Kelly M.; Kwak N.; Lam H.; Kubota Y.; Lattery M.; Nelson J.; Patton S.; Perticone D.; Poling R.; Savinov V.; Schrenk S.; Wang R.; Alam M.; Kim I.; O'Neill J.; Nemati B.; Romero V.; Severini H.; Sun C.; Wang P.; Zoeller M.; Crawford G.; Fulton R.; Gan K.; Kagan H.; Kass R.; Lee J.; Malchow R.; Morrow F.; Sung M.; White C.; Whitmore J.; Wilson P.; Butler F
Axisymmetric oscillations at L-H transitions in JET: M-mode
No full textL to H transition studies at JET have revealed an n = 0, m = 1 magnetic oscillation starting immediately at the L to H transition (called M-mode for brevity). While the magnetic oscillation is present a weak ELM-less H-mode regime is obtained, with a clear increase of density and a weak electron temperature pedestal. It is an intermediate state between L and H-mode. In ICRH heated plasmas or low density NBI plasmas the magnetic mode and the pedestal can remain steady (with small oscillations) for the duration of the heating phase, of order 10 s or more. The axisymmetric magnetic oscillation has period ∼0.5-2 ms, and poloidal mode number m = 1: it looks like a pedestal localised up/down oscillation, although it is clearly a natural oscillation of the plasma, not driven by the position control system. Electron cyclotron emission, interferometry, reflectometry and fast Li beam measurements locate the mode in the pedestal region. Dα, fast infrared camera and Langmuir probe measurements show that the mode modulates heat and particle fluxes to the target. The mode frequency appears to scale with the poloidal Alfvén velocity, and not with sound speed (i.e. it is not a geodesic acoustic mode). A heuristic model is proposed for the frequency scaling of the mode. We discuss the relationship between the M-mode and other related observations near the L-H transition
Analysis of hadronic transitions in Υ(3S) decays
No full textComplete Author List: Butler, F.; Fu, X.; Kalbfleisch, G.; Lambrecht, M.; Ross, W.R.; Skubic, P.; Snow, J.; Wang, P.L.; Wood, M.; Bortoletto, D.; Brown, D.N.; Fast, J.; McIlwain, R.L.; Miao, T.; Miller, D.H.; Modesitt, M.; Schaffner, S.F.; Shibata, E.I.; Shipsey, I.P.J.; Wang, P.N.; Battle, M.; Ernst, J.; Kroha, H.; Roberts, S.; Sparks, K.; Thorndike, E.H.; Wang, C.H.; Dominick, J.; Sanghera, S.; Skwarnicki, T.; Stroynowski, R.; Artuso, M.; He, D.; Goldberg, M.; Horwitz, N.; Kennett, R.; Moneti, G.C.; Muheim, F.; Mukhin, Y.; Playfer, S.; Rozen, Y.; Stone, S.; Thulasidas, M.; Vasseur, G.; Zhu, G.; Bartelt, J.; Csorna, S.E.; Egyed, Z.; Jain, V.; Sheldon, P.; Akerib, D.S.; Barish, B.; Chadha, M.; Chan, S.; Cowen, D.F.; Eigen, G.; Miller, J.S.; O'Grady, C.; Urheim, J.; Weinstein, A.J.; Acosta, D.; Athanas, M.; Masek, G.; Paar, H.; Sivertz, M.; Bean, A.; Gronberg, J.; Kutschke, R.; Menary, S.; Morrison, R.J.; Nakanishi, S.; Nelson, H.N.; Nelson, T.K.; Richman, J.D.; Ryd, A.; Tajima, H.; Schmidt, D.; Sperka, D.; Witherell, M.S.; Procario, M.; Yang, S.; Balest, R.; Cho, K.; Daoudi, M.; Ford, W.T.; Johnson, D.R.; Lingel, K.; Lohner, M.; Rankin, P.; Smith, J.G.; Alexander, J.P.; Bebek, C.; Berkelman, K.; Besson, D.; Browder, T.E.; Cassel, D.G.; Cho, H.A.; Coffman, D.M.; Drell, P.S.; Ehrlich, R.; Galik, R.S.; Garcia-Sciveres, M.; Geiser, B.; Gittelman, B.; Gray, S.W.; Hartill, D.L.; Heltsley, B.K.; Jones, C.D.; Jones, S.L.; Kandaswamy, J.; Katayama, N.; Kim, P.C.; Kreinick, D.L.; Ludwig, G.S.; Masui, J.; Mevissen, J.; Mistry, N.B.; Ng, C.R.; Nordberg, E.; Ogg, M.; Patterson, J.R.; Peterson, D.; Riley, D.; Salman, S.; Sapper, M.; Worden, H.; Wuerthwein, F.; Avery, P.; Freyberger, A.; Rodriguez, J.; Stephens, R.; Yelton, J.; Cinabro, D.; Henderson, S.; Kinoshita, K.; Liu, T.; Saulnier, M.; Shen, F.; Wilson, R.; Yamamoto, H.; Ong, B.; Selen, M.; Sadoff, A.J.; Ammar, R.; Ball, S.; Baringer, P.; Coppage, D.; Copty, N.; Davis, R.; Hancock, N.; Kelly, M.; Kwak, N.; Lam, H.; Kubota, Y.</p
Apamea commixta Butler 1881
No full textApamea commixta (Butler, 1881) (Figs 2, 5, 7) Xylophasia commixta Butler, 1881. Trans. ent. Soc. London. 1881: 174 (Type locality: Japan, Yokohama, Tokyo). Xylophasia tychoona Leech, 1889. Proc. zool. Soc. Lond. 1889: 488, Pl. 51: 3, (Type locality: not stated [Japan]). Hampson, 1908: 178, pl. CXII: 16 (Trachea commixta); Warren, 1914: 169, Taf. 40 e (Parastichtis commixta); Inoue & Sugi, 1958: 491 (Apamea commixta); Sugi, 1982; 1989: 1055 (Apamea commixta). This little known species is distributed in Japan (Hokkaido and Honshu Isl.) (Inoue and Sugi 1958; Sugi 1989), South Kurile Island (Kunashir and Iturup), and South Sakhalin (Kononenko 2005). The type specimens of Xylophasia commixta Butler and Xylophasia tychoona Leech are illustrated by Krusek & Behounek (1996). The imago and male genitalia of A. commixta are illustrated by Sugi (1982). The species inhabits grassy meadows and low grassland hills along the seashore (Marusik, pers. comm.). Material examined. 3 males: Japan, Japanese Alps, 4 Aug 1914 (H. Höne); 3 males, Japan, Kamikoshi, 1600 m, Japanese Alps, Aug 1914 (H. Höne), genit. prep. ZFMK 1830 VK.; 1 female, Japan, Yokohama, 2 Aug 1937 (H. Höne), genit. prep. VSK 10 / 050698, ZFMK; 3 males and 1 female, Russia, Kurile Isl., Iturup I., 45 ° 20 ' N, 147 ° 59 ' 8 " E, Konservnaya Bay, 12–16 Aug 1995 (Yu. Marusik); 2 males, Russia, Kunashir Isl., SW of Yuznokurilsk, Lesnaya River, 44 ° 00' 72 " N, 145 ° 46 ' 28 " E, 1 Sep 1995 (Yu. Marusik), IBSS; 2 females, Russia, South Sakhalin, 25 km NE Aniva, 10–18 Aug 1985 (A. Danchenko), ZFMK.Published as part of Kononenko, Vladimir, 2006, Apamea permixta, sp. n., from China — the putative sister species of A. commixta (Butler) (Lepidoptera, Noctuidae: Xyleninae: Apameini), pp. 37-43 in Zootaxa 1371 on page 42, DOI: 10.5281/zenodo.17493
Estimation of interdomain flexibility of N-terminus of factor H using residual dipolar couplings
No full textCharacterization of segmental flexibility is needed to understand the biological mechanisms of the very large category of functionally diverse proteins, exemplified by the regulators of complement activation, that consist of numerous compact modules or domains linked by short, potentially flexible, sequences of amino acid residues. The use of NMR-derived residual dipolar couplings (RDCs), in magnetically aligned media, to evaluate interdomain motion is established but only for two-domain proteins. We focused on the three N-terminal domains (called CCPs or SCRs) of the important complement regulator, human factor H (i.e., FH1-3). These domains cooperate to facilitate cleavage of the key complement activation-specific protein fragment, C3b, forming iC3b that no longer participates in the complement cascade. We refined a three-dimensional solution structure of recombinant FH1-3 based on nuclear Overhauser effects and RDCs. We then employed a rudimentary series of RDC data sets, collected in media containing magnetically aligned bicelles (disklike particles formed from phospholipids) under three different conditions, to estimate interdomain motions. This circumvents a requirement of previous approaches for technically difficult collection of five independent RDC data sets. More than 80% of conformers of this predominantly extended three-domain molecule exhibit flexions of <40°. Such segmental flexibility (together with the local dynamics of the hypervariable loop within domain 3) could facilitate recognition of C3b via initial anchoring and eventual reorganization of modules to the conformation captured in the previously solved crystal structure of a C3b:FH1-4 complex.</p
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