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  • Geophysics  (2)
  • diet-mixing  (2)
  • 5-Azacytidine  (1)
  • 1
    Electronic Resource
    Electronic Resource
    Amsterdam : Elsevier
    Journal of Insect Physiology 33 (1987), S. 77-82 
    ISSN: 0022-1910
    Keywords: Supella longipalpa ; brown-banded cockroach ; diet-mixing ; nutrient self-selection ; nutritional physiology
    Source: Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
    Topics: Biology
    Type of Medium: Electronic Resource
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  • 2
    Electronic Resource
    Electronic Resource
    Amsterdam : Elsevier
    Mutation Research DNA Repair Reports 193 (1988), S. 229-236 
    ISSN: 0167-8817
    Keywords: 5-Azacytidine ; Escherichia coli ; Methyltransferase genes
    Source: Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
    Topics: Biology , Medicine
    Type of Medium: Electronic Resource
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  • 3
    Electronic Resource
    Electronic Resource
    Springer
    Entomologia experimentalis et applicata 44 (1987), S. 65-73 
    ISSN: 1570-7458
    Keywords: nutrient self-selection ; diet-mixing ; Heliothis zea ; feeding behavior ; nutrition
    Source: Springer Online Journal Archives 1860-2000
    Topics: Biology
    Description / Table of Contents: Résumé Récemment nous avions montré que les chenilles du dernier stade d'H. zea (Boddie) (Lep.: Noctuidae) composaient elles-mêmes leurs repas à partir de 2 cubes d'aliments, l'un carencé en protéine (caséine), l'autre en carbohydrate assimilable (sucrose). Dans cette nouvelle étude, les témoins ont reçu deux cubes nutritivement complets et les lots expérimentaux (en auto-complexification) deux cubes nutritivement incomplets, l'un carencé en caséine, l'autre en sucrose. Les chenilles ont traversé 3 étapes pendant ce dernier stade; une phase initiale de perturbations durant laquelle elles ne mangeaient presque pas, mais changeaient souvent de cube, une phase d'installation pendant laquelle elles consommainet d'une façon plus ou moins continue; et une phase de prénymphose pendant laquelle elles vagabondaient. La phase perturbée était moins longue chez les témoins, mais les deux lots présentaient le même comportement pendant cette phase: changeant de cube jusqu' à neuf fois par heure. Dès que la prise d'aliment a commencé dans la phase installée, les témoins changeaient de cube au hasard, tandis que les chenilles en expérience en changeaient relativement plus, passant 17% de leur temps sur le sucrose et 83% sur la caséine. Les comportements étaient identiques chez les deux lots pendant la phase de prénymphose. L'autocomplexification correspond à un comportement particulier pendant le dernier stade: l'alimentation sur caséine domine tôt, elle tend ensuite à rester constante tandis que l'alimentation sur caséine est maximale vers la fin du stade. Notre hypothèse est que l'auto-complexification est gouvernée par des feedbacks physiologiques internes déterminant la prise d'aliments, et que la chenille peut apprendre à associer un goût à un contenu nutritif.
    Notes: Abstract When presented with two nutritionally incomplete diets, one lacking only the protein (casein) and the other lacking only the digestible carbohydrate (sucrose), last instar larvae of Heliothis zea (Boddie) (Lepidoptera: Noctuidae) switched between the diets frequently. The ratio (casein:sucrose) of time they spent on the two diets was about 83:17. As the stadium proceeded, the relative time they spent on the sucrose diet increased. Control larvae, offered two identical, nutritionally complete diets, seldom switched between them.
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  • 4
    Publication Date: 2019-07-10
    Description: Observations obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE) have been used to determine the column densities of D I, O I, and N I along seven sight lines that probe the local interstellar medium (LISM) at distances from 37 pc to 179 pc. Five of the sight lines are within the Local Bubble and two penetrate the surrounding H I wall. Reliable values of N(H I) were determined for five of the sight lines from HST data, IUE data, and published EUVE measurements. The weighted mean of DI/H I for these five sight lines is (1.52 +/- 0.08) x l0(exp -5)(1 sigma uncertainty in the mean). It is likely that the D I/H I ratio in the Local Bubble has a single value. The D I/O I ratio for the five sight lines within the Local Bubble is (3.76 +/- 0.20) x 10(esp -2). It is likely that O I column densities can serve as a proxy for H I in the Local Bubble. The weighted mean for O I/ H I for the seven FUSE sight lines is (3.03 +/- 0.21) x 10(esp -4), comparable to the weighted mean (3.43 +/- 0.15) x 10(exp -4) reported for 13 sight lines probing larger distances and higher column densities. The FUSE weighted mean of N I/ H I for five sight lines is half that reported by Meyer et al. for seven sight lines with larger distances and higher column densities. This result combined with the variability of O I/ N I (six sight lines) indicates that at the low column densities found in the LISM, nitrogen ionization balance is important. Thus, unlike O I, N I cannot be used as a proxy for H I or as a metallicity indicator in the LISM.
    Keywords: Geophysics
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  • 5
    Publication Date: 2019-07-10
    Description: We present measurements of the column densities of interstellar D I and O I made with the Far Ultraviolet Spectroscopic Explorer (FUSE), and of H I made with the International Ultraviolet Explorer (IUE) toward the sdOB star Feige 110 [(l,b) = (74.09 deg., - 59.07 deg.); d = 179(sup +265, sub -67) pc; Z = -154(sup +57, Sub -227 pc). Our determination of the D I column density made use of curve of growth fitting and profile fitting analyses, while our O I column density determination used only curve of growth techniques. The H I column density was estimated by fitting the damping wings of the interstellar Ly(lpha) profile. We find log N(D I) = 15.47 +/- 0.06, log N(O I) = 16.73 +/- 0.10, and log N(H I) = 20.14(sup +0.13, sub -0.20) (all errors 2(sigma)). This implies D/H = (2.14 +/- 0.82) x 10(esp -5), D/O = (5.50(sup + 1.64, sub -133)) x 10(exp -2), and O/H = (3.89 +/- 1.67) x 10(exp -4). Taken with the FUSE results reported in companion papers and previous measurements of the local interstellar medium, this suggests the possibility of spatial variability in D/H for sight lines exceeding approx. 100 pc. This result may constrain models which characterize the mixing time and length scales of material in the local interstellar medium.
    Keywords: Geophysics
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