Sequential origin in the high performance properties of spider dragline silk

Major ampullate (MA) dragline silk supports spider orb webs, combining strength and extensibility in the toughest biomaterial. MA silk evolved ~376 MYA and identifying how evolutionary changes in proteins influenced silk mechanics is crucial for biomimetics, but is hindered by high spinning plasticity. We use supercontraction to remove that variation and characterize MA silk across the spider phylogeny. We show that mechanical performance is conserved within, but divergent among, major lineages, evolving in correlation with discrete changes in proteins. Early MA silk tensile strength improved rapidly with the origin of GGX amino acid motifs and increased repetitiveness. Tensile strength then maximized in basal entelegyne spiders, ~230 MYA. Toughness subsequently improved through increased extensibility within orb spiders, coupled with the origin of a novel protein (MaSp2). Key changes in MA silk proteins therefore correlate with the sequential evolution high performance orb spider silk and could aid design of biomimetic fibers.

Minor ampullate silks from Nephila and Argiope spiders: tensile properties and microstructural characterization

The mechanical behavior and microstructure of minor ampullate gland silk (miS) of two orb-web spinning species, Argiope trifasciata and Nephila inaurata, were extensively characterized, enabling detailed comparison with other silks. The similarities and differences exhibited by miS when compared with the intensively studied major ampullate gland silk (MAS) and silkworm (Bombyx mori) silk offer a genuine opportunity for testing some of the hypotheses proposed to correlate microstructure and tensile properties in silk. In this work, we show that miSs of different species show similar properties, even when fibers spun by spiders that diverged over 100 million years are compared. The tensile properties of miS are comparable to those of MAS when tested in air, significantly in terms of work to fracture, but differ considerably when tested in water. In particular, miS does not show a supercontraction effect and an associated ground state. In this regard, the behavior of miS in water is similar to that of B. mori silk, and it is shown that the initial elastic modulus of both fibers can be explained using a common model. Intriguingly, the microstructural parameters measured in miS are comparable to those of MAS and considerably different from those found in B. mori. This fact suggests that some critical microstructural information is still missing in our description of silks, and our results suggest that the hydrophilicity of the lateral groups or the large scale organization of the sequences might be routes worth exploring.

The variability and interdependence of spider viscid line tensile properties

True stress-true strain curves of naturally spun viscid line fibers retrieved directly from the spiral of orb-webs built by Argiope trifasciata spiders were measured using a novel methodology. This new procedure combines a method for removing the aqueous coating of the fibers and a technique that allows the accurate measurement of their cross sectional area. Comparison of the tensile behaviour of different samples indicates that naturally spun viscid lines show a large variability, comparable to that of other silks, such as major ampullate gland silk and silkworm silk. Nevertheless, application of a statistical analysis allowed identifying two independent parameters that underlie the variability and characterize the observed range of true stress-true strain curves. Combination of this result with previous mechanical and microstructural data suggested the assignment of these two independent effects to the degree of alignment of the protein chains and to the local relative humidity which, in turn, depends on the composition of the viscous coating and on the external environmental conditions.

Astrophysical parameters of LS 2883 and implications for the PSR B1259-63 gamma-ray binary

Only a few binary systems with compact objects display TeV emission. The physical properties of the companion stars represent basic input for understanding the physical mechanisms behind the particle acceleration, emission, and absorption processes in these so-called gamma-ray binaries. Here we present high-resolution and high signal-to-noise optical spectra of LS 2883, the Be star forming a gamma-ray binary with the young non-accreting pulsar PSR B1259-63, showing it to rotate faster and be significantly earlier and more luminous than previously thought. Analysis of the interstellar lines suggests that the system is located at the same distance as (and thus is likely a member of) Cen OB1. Taking the distance to the association, d = 2.3 kpc, and a color excess of E(B – V) = 0.85 for LS 2883 results in MV ≈ –4.4. Because of fast rotation, LS 2883 is oblate (R eq sime 9.7 R ☉ and R pole sime 8.1 R ☉) and presents a temperature gradient (T eq≈ 27,500 K, log g eq = 3.7; T pole≈ 34,000 K, log g pole = 4.1). If the star did not rotate, it would have parameters corresponding to a late O-type star. We estimate its luminosity at log(L */L ☉) sime 4.79 and its mass at M * ≈ 30 M ☉. The mass function then implies an inclination of the binary system i orb ≈ 23°, slightly smaller than previous estimates. We discuss the implications of these new astrophysical parameters of LS 2883 for the production of high-energy and very high-energy gamma rays in the PSR B1259-63/LS 2883 gamma-ray binary system. In particular, the stellar properties are very important for prediction of the line-like bulk Comptonization component from the unshocked ultrarelativistic pulsar wind.

Orexin-stimulated MAP kinase cascades are activated through multiple G-protein signalling pathways in human H295R adrenocortical cells: diverse roles for orexins A and B

Orexins A and B (ORA and ORB) are neuropeptide hormones found throughout the central nervous system and periphery. They are required for a host of physiological processes including mitogen-activated protein kinase (MAPK) regulation, steroidogenesis, appetite control and energy regulation. While some signalling mechanisms have been proposed for individual recombinant orexin receptors in generic mammalian cell types, it is clear that the peripheral effects of orexin are spatially and temporally complex. This study dissects the different G-protein signalling and MAPK pathways activated in a pluripotent human adrenal H295R cell line capable of all the physiological steps involved in steroidogenesis. Both extracellular receptor kinase 1/2 (ERK1/2) and p38 were phosphorylated rapidly with a subsequent decline, in a time- and dose-dependent manner, in response to both ORA and ORB. Conversely, there was little or no direct activation of the ERK5 or JNK pathway. Analysis using signalling and MAPK inhibitors as well as receptor-specific antagonists determined the precise mediators of the orexin response in these cells. Both ERK1/2 and p38 activation were predominantly Gq- and to a lesser extent Gs-mediated; p38 activation even had a small Gi-component. Effects were broadly comparable for both orexin sub-types ORA and ORB and although most of the effects were transmitted through the orexin receptor-1 subtype, we did observe a role for orexin receptor-2-mediated activation of both ERK1/2 and p38. Cortisol secretion also differed in response to ORA and ORB. These data suggest multiple roles for orexin-mediated MAPK activation in an adrenal cell-line, this complexity may help to explain the diverse biological actions of orexins with wide-ranging consequences for our understanding of the mechanisms initiated by these steroidogenic molecules.

OCT retinal thickness ratios and frequency of follow-up in Wet AMD

Poster Introduction: In neovascular age-related macular degeneration (nAMD), optical coherence tomography (OCT) is an important tool to determine when intravitreal injections of ranibizumab should be administered. Current guidelines recommend that patients should be reviewed four weekly and OCT indications for further treatment include subretinal fluid and intraretinal fluid or cysts. Purpose: We have reviewed the OCT scans of subjects who have successfully responded to ranibizumab to look for factors that might predict which patients will not require injection and could have extended appointments. Method: This was a prospective study in which we observed for 6 consecutive months the OCT images of 28 subjects who had received intravitreal ranibizumab for nAMD and were judged to be clinically inactive at recruitment to the study. Ratios between full retinal thickness (FRT = neurosensory retina + outer reflective band) and outer reflective band (ORB) thickness at the fovea were calculated for each subject at the moment of entering the study and at each successive visit for 6 consecutive months. Results: Patients with lower FRT/ORB ratios were found to be less likely to require an additional injection of ranibizumab and no subject with a ratio of 1.75 or less needed further injections. Conclusion: This small pilot study suggests that on macular OCT, the FRT/ORB ratio, and in particular values of 1.75 or less, may prove to be a useful, practical tool when deciding the follow up period for subjects undergoing treatment with intravitreal ranibizumab for nAMD.

The VLT-FLAMES Tarantula Survey XXI. Stellar spin rates of O-type spectroscopic binaries

Context: The initial distribution of spin rates of massive stars is a fingerprint of their elusive formation process. It also sets a key initial condition for stellar evolution and is thus an important ingredient in stellar population synthesis. So far, most studies have focused on single stars. Most O stars are, however, found in multiple systems. 

Aims: By establishing the spin-rate distribution of a sizeable sample of O-type spectroscopic binaries and by comparing the distributions of binary subpopulations with one another and with that of presumed-single stars in the same region, we aim to constrain the initial spin distribution of O stars in binaries, and to identify signatures of the physical mechanisms that affect the evolution of the spin rates of massive stars. 

Methods: We use ground-based optical spectroscopy obtained in the framework of the VLT-FLAMES Tarantula Survey (VFTS) to establish the projected equatorial rotational velocities (ν_esini) for components of 114 spectroscopic binaries in 30 Doradus. The ν_esini values are derived from the full width at half maximum (FWHM) of a set of spectral lines, using a FWHM vs. ν_esini calibration that we derive based on previous line analysis methods applied to single O-type stars in the VFTS sample. 

Results: The overall ν_esini distribution of the primary stars resembles that of single O-type stars in the VFTS, featuring a low-velocity peak (at ν_esini<200 kms^-1) and a shoulder at intermediate velocities (200 <ν_esini<300 kms^-1). The distributions of binaries and single stars, however, differ in two ways. First, the main peak at ν_esini ~ 100kms^-1 is broader and slightly shifted towards higher spin rates in the binary distribution than that of the presumed-single stars. This shift is mostly due to short-period binaries (P_orb~<10 d). Second, the ν_esini distribution of primaries lacks a significant population of stars spinning faster than 300 kms^-1, while such a population is clearly present in the single-star sample. The ν_esini distribution of binaries with amplitudes of radial velocity variation in the range of 20 to 200 kms^-1 (mostly binaries with P_orb ~ 10-1000 d and/or with q<0.5) is similar to that of single O stars below ν_esini_~<170kms^-1. 

Conclusions: Our results are compatible with the assumption that binary components formed with the same spin distribution as single stars, and that this distribution contains few or no fast-spinning stars. The higher average spin rate of stars in short-period binaries may either be explained by spin-up through tides in such tight binary systems, or by spin-down of a fraction of the presumed-single stars and long-period binaries through magnetic braking (or by a combination of both mechanisms). Most primaries and secondaries of SB2 systems with P_orb~<10 d appear to have similar rotational velocities. This is in agreement with tidal locking in close binaries where the components have similar radii. The lack of very rapidly spinning stars among binary systems supports the idea that most stars with ν_esini_~> 300kms^-1 in the single-star sample are actually spun-up post-binary interaction products. Finally, the overall similarities (low-velocity peak and intermediate-velocity shoulder) of the spin distribution of binary and single stars argue for a massive star formation process in which the initial spin is set independently of whether stars are formed as single stars or as components of a binary system.

Mikrofaunistisch-lithologische Untersuchungen der Hilssandstein-Region (Apt/Alb) im Raum Salzgitter-Goslar

So gut sich im nördlichen Harzvorland die Sandstein- Fazies des Hilssandsteins als morphologisch herausragende Schichtrippe kartieren ließ, so problematisch ist bis heute ihre genaue stratigraphische Position geblieben. Die von STROMBECK (1856, Tab.S.493) aufgestellten Schichtgruppen Hilssandstein und Minimuston verwendete noch STOLLEY (1937, S.1,54) in stratigraphischem Sinn, obgleich es sich um Fazieseinheiten handelt, deren Grenzen durchaus schräg zu den biostratigraphischen Zonen verlaufen können. Beispiele für die Richtigkeit dieses Prinzips lieferten die Beobachtungen am Flammenmergel des Hils und der Sackmulde (JORDAN & SCHMIDT 1968): Die Bildungszeit der Flammenmergel-Fazies beginnt nach neuer Zonengliederung (COLLIGNON 1965) nicht zugleich mit dem Ober-Alb, sindern erst im unteren Ober-Alb und reicht bis zum Cenoman, kann aber auch schon im Ober-Alb beendet sein. Ein ähnliches Verhalten wurde daher auch von der Quarzsandstein-Fazies des Hilssandsteins im Raum Salzgitter-Goslar vermutet. Seltene Vorkommen von Acanthohoplites milletianus D'ORB. in den Steinbrüchen von Ostlutter und in der Sandgrube bei Goslar waren für BODE & SCHROEDER (1912 - 1926) bei ihrer geologischen Kartenaufnahme der Beweis für Unter-Gault (= Unter-Alb) -Alter des Sandsteins. Bei der Auswertung der Bohrungen im Gebiet von Hornburg grenzte SEITZ (1943, S.355,398) die Quarzsandstein Fazies mit dem Gaultkonglomerat nach unten gegen tonige Apt-Serien ab und stellte die obere Faziesgrenze des Hilssandsteins gegen Minimuston nach einem Leymeriellen Fund etwa in die Mitte des oberen Unter-Albs. Weiter östlich durchgeführte mikropaläontologische Beobach- tungsn in der Unterkreide am Kleinen Fallstein (BACH 1965) bestätigten, daß hier die Quarzsandschüttung bereits im Unter-Alb beendet war. Im Westen des Untersuchungsgebietes soll die Quarzsandschüttung im Hils nach BRINKMANN (1937, S.15) im Ober-Apt, örtlich sogar im Ober-Hauterive (FRATSCHNER 1950, S.31) begonnen und nach einem Hoplites-Fund (BRINKMANN 1937, S.15) bis ins oberste Mittel-Alb angedauert haben. Den Hilssandstein der Sackmulde stell- tein JORDAN & SCHMIDT (1968, S.428) ins Unter-Alb, vermuteten aber dessen Sedimentationsbeginn im Ober-Apt. Im Untersuchungsgebiet dieser Arbeit wurde das Unter- Alb-Alter des Hilssandsteins von DEWIEL (1951, S.39) unter anderem in der Finkeikuhle (bei Salzgitter-Bad) angezweifeit: Seines Erachtens ist dort die gesamte, ungefähr 50 m mächtige, tonig-sandige Folge mit Sandsteinbänken in ihrem oberen Teil dem Ober-Apt zuzuordnen. Er unterstrich damit WEIGELTs (1923, S.44/45) Auffassung von einer zumindest partiellen Zugehörigkeit des Sandsteins zum hohen Neokom. Abgesehen von der guten Übereinstimmung in der Datierung der Hilssandstein-Region des Kleinen Fallsteins nach Makro- wie Mikrofauna, gaben die zum Teil widersprüchlichen Altersangaben für dieselbe Schichtregion in den anderen Gebieten Südniedersachsens Anlaß zur Skepsis. Das hiesige Institut machte es sich daher zur Aufgabe, die stratigraphische Stellung des Hilssandsteins zunächst im Hils (SEILER 1973) und im Raum Salzgitter-Goslar erneut zu untersuchen. Die hier bearbeiteten Aufschlüsse (Abb.l) (Bl. Ringelheim, Salzgitter, Lutter a.B., Goslar) liegen im wesentlichen im Ausstrich der Unterkreide an den Flanken der Innerste-Mulde (gelegentlich auch Ringelheimer Mulde genannt). Bekanntlich entstand diese asymmetrische, mit Kreide-Sedimenten gefüllte Mulde durch halokinetisch modifizierte junge (?subherzynische) tektonische Bewegungen (s. KÖLBEL 1944). An ihrer Westflanke und in der Harzrandzone westlich Goslar bildet der Hilssandstein eine Schichtrippe und überlagert transgressiv Trias- und Jura-Schichten. - An seiner Basis treten örtlich (z.B. SO Ortshausen, SW Neuwallmoden) geringmächtige Brauneisenstein-Phosphorit- Lagen auf, deren Zugehörigkeit zum Neokom- oder Gaultkonglomerat bisher nicht sicher war. An der östlichen Muldenflanke ist der Hilssandstein in Tagesaufschlüssen aus zwei Gebieten bekannt: a) im Kreuzungsbereich der rheinisch streichenden Ringel- heimer Störungszone (KÖLBEL 1944, S.82) mit dem eggisch bis steil-herzynisch streichenden Salzgitterer Sattel in der Umgebung von Gitter und Grube "Finkeikuhle", b) am Südende des Salzgitterer Sattels. - Hier, wie auch am Südteil der östlichen Sattelflanke bei Groß-Döhren und Weddingen (Aufschluß 5: "Morgenstern"), liegt der Hilssandstein samt Gaultkonglomerat transgressiv auf den erzführenden Serien der tieferen Unterkreide.

Assessment of surface temperatures of buffalo bulls (Bubalus bubalis) raised under tropical conditions using infrared thermography.

O presente trabalho visou avaliar as temperaturas superficiais de diferentes regiões anatômicas de búfalos ao longo do tempo, por meio da termografia infravermelha, e correlacioná-las a índices bioclimatológicos de conforto térmico. O ensaio foi realizado em região de clima tropical úmido (Afi de Köppen), de abril a agosto. Dez touros (n=10) foram avaliados a cada 25 dias (manhã: seis-nove horas; tarde: 12-15h), quanto à frequência respiratória (FR), temperatura retal (TR) e imagens termográficas da órbita ocular (ORB), flanco direito (FLd), flanco esquerdo (FLe) e escroto (ESC). Os dados climatológicos foram ininterruptamente monitorados, e calculados o índice de temperatura e umidade (ITU) e o índice de conforto de Benezra (ICB). O ITU foi ?78, com diferença entre turnos (P<0,05). Já o ICB variou de 1,96 a 2,25 e apresentou diferenças ao longo dos meses e entre turnos (P<0,05). As temperaturas observadas foram de TR=38,2±0,5ºC, ORB=36,1±0,8ºC, FLd=33,5±2,5ºC, FLe=35,4±1,7ºC e ESC=33,3±1,1ºC, as quais variaram significativamente ao longo dos meses e entre turnos (P<0,05). O ITU apresentou correlações positivas com ORB (0,72), FLd (0,77), FLe (0,75) e ESC (0,41) (P<0,0001). A temperatura máxima de ORB apresentou a maior correlação com a TR (0,58; P<0,0001). Portanto, as temperaturas superficiais dos animais sofrem interferências das variações climáticas e se elevam ao longo do dia, devido à variação nos índices de conforto térmico; a temperatura máxima de ORB foi o parâmetro mais condicionado à temperatura retal. Também, as oscilações de temperatura de superfície de ORB, FLd, FLe e ESC podem ser aferidas em bubalinos com o uso da termografia infravermelha, de modo preciso e não invasivo.

Assessment of surface temperatures of buffalo bulls (Bubalus bubalis) raised under tropical conditions using infrared thermography.

O presente trabalho visou avaliar as temperaturas superficiais de diferentes regiões anatômicas de búfalos ao longo do tempo, por meio da termografia infravermelha, e correlacioná-las a índices bioclimatológicos de conforto térmico. O ensaio foi realizado em região de clima tropical úmido (Afi de Köppen), de abril a agosto. Dez touros (n=10) foram avaliados a cada 25 dias (manhã: seis-nove horas; tarde: 12-15h), quanto à frequência respiratória (FR), temperatura retal (TR) e imagens termográficas da órbita ocular (ORB), flanco direito (FLd), flanco esquerdo (FLe) e escroto (ESC). Os dados climatológicos foram ininterruptamente monitorados, e calculados o índice de temperatura e umidade (ITU) e o índice de conforto de Benezra (ICB). O ITU foi ?78, com diferença entre turnos (P<0,05). Já o ICB variou de 1,96 a 2,25 e apresentou diferenças ao longo dos meses e entre turnos (P<0,05). As temperaturas observadas foram de TR=38,2±0,5ºC, ORB=36,1±0,8ºC, FLd=33,5±2,5ºC, FLe=35,4±1,7ºC e ESC=33,3±1,1ºC, as quais variaram significativamente ao longo dos meses e entre turnos (P<0,05). O ITU apresentou correlações positivas com ORB (0,72), FLd (0,77), FLe (0,75) e ESC (0,41) (P<0,0001). A temperatura máxima de ORB apresentou a maior correlação com a TR (0,58; P<0,0001). Portanto, as temperaturas superficiais dos animais sofrem interferências das variações climáticas e se elevam ao longo do dia, devido à variação nos índices de conforto térmico; a temperatura máxima de ORB foi o parâmetro mais condicionado à temperatura retal. Também, as oscilações de temperatura de superfície de ORB, FLd, FLe e ESC podem ser aferidas em bubalinos com o uso da termografia infravermelha, de modo preciso e não invasivo.