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1. Effects of aflatoxin B1, fumonisin B1 and their mixture on the aryl hydrocarbon receptor and cytochrome P450 1A induction

Author: Mary, V. S., Valdehita Torija, Ana, Navas Antón, José María, Rubinstein, H. R., Fernández-Cruz, M. L., Mary, V. S., Valdehita Torija, Ana, Navas Antón, José María, Rubinstein, H. R., and Fernández-Cruz, M. L.
Abstract: Aflatoxin B1 (AFB1) and fumonisin B1 (FB1) are mycotoxins widely found as cereal contaminants and their co-occurrence in corn has been associated with a high incidence of liver cancer. Both toxins are immunotoxic, with AFB1 being a procarcinogen, and its bioactivation through specific cytochrome P450 (Cyp) enzymes, such as Cyp1A, being a requirement for hepatocarcinogenic and toxic activities. This study evaluated the effects of these mycotoxins, alone or combined, on activation and expression of Cyp1A and its transcription factor aryl hydrocarbon receptor (Ahr) in hepatoma cell line H4IIE and spleen mononuclear cells of rats. The results demonstrate that in H4IIE cells, AFB1 induced an increase in Cyp1A activity and cyp1A transcription, associated with an enhanced Ahr activity, which suggests that this toxin can act as an Ahr agonist. Moreover, FB1 caused a small rise in Cyp1A activity and cyp1A expression. Similarly in spleen cells, AFB1 and FB1 induced overexpression of cyp1A and ahr genes. This work shows that the response potency was significantly higher for the mixture, indicating the existence of an interaction between both toxins. This study proposes the Ahr pathway activation as a toxicity mechanism of AFB1 and FB1, and highlights that FB1 may increase AFB1 bioactivation. © 2014 Elsevier Ltd.
Published: 2015

2. Minimal triangulations for an infinite family of lens spaces

Author: Jaco, W, Rubinstein, H, Tillmann, S, Jaco, W, Rubinstein, H, and Tillmann, S
Published: 2009

3. Recent results from AMANDA

Author: Andrés, E., Askebjer, P., Bai, X., Barouch, G., Barwick, S. W., Bay, R. C., Becker, K. -H, Bergström, L., Bertrand, D., Bierenbaum, D., Biron, A., Booth, J., Botner, O., Bouchta, A., Boyce, M. M., Carius, Staffan, Chen, A., Chirkin, D., Conrad, J., Cooley, J., Costa, C. G. S., Cowen, D. F., Dailing, J., Dalberg, E., De Young, T., Desiati, P., Dewulf, J. -P, Doksus, P., Edsjö, J., Ekström, P., Erlandsson, B., Feser, T., Gaug, M., Goldschmidt, A., Goobar, A., Gray, L., Haase, H., Hallgren, A., Halzen, F., Hanson, K., Hardtke, R., He, Y. D., Hellwig, M., Heukenkamp, H., Hill, G. C., Hulth, P. O., Hundertmark, S., Jacobsen, J., Kandhadai, V., Karle, A., Kim, J., Koci, B., Köpke, L., Kowalski, M., Leich, H., Leuthold, M., Lindahl, P., Liubarsky, I., Loaiza, P., Lowder, D. M., Ludvig, J., Madsen, J., Marciniewski, P., Matis, H. S., Mihalyi, A., Mikolajski, T., Miller, T. C., Minaeva, Y., Miočinović, P., Mock, P. C., Morse, R., Neunhöffer, T., Newcomer, F. M., Niessen, P., Nygren, D. R., Ogelman, H., Pérez De Los Heros, C., Porrata, R., Price, P. B., Rawlins, K., Reed, C., Rhode, W., Richards, A., Richter, S., Rodríguez Martino, J., Romenesko, P., Ross, D., Rubinstein, H., Sander, H. -G, Scheider, T., Schmidt, T., Schneider, D., Schneider, E., Schwarz, R., Silvestri, A., Solarz, M., Spiczak, G. M., Spiering, C., Starinsky, N., Steele, D., Steffen, P., Stokstad, R. G., Streicher, O., Sun, Q., Taboada, I., Thollander, L., Thon, T., Tilav, S., Usechak, N., Vander Donckt, M., Walck, C., Weinheimer, C., Wiebusch, C. H., Wischnewski, R., Wissing, H., Woschnagg, K., Wu, W., Yodh, G., Young, S., Andrés, E., Askebjer, P., Bai, X., Barouch, G., Barwick, S. W., Bay, R. C., Becker, K. -H, Bergström, L., Bertrand, D., Bierenbaum, D., Biron, A., Booth, J., Botner, O., Bouchta, A., Boyce, M. M., Carius, Staffan, Chen, A., Chirkin, D., Conrad, J., Cooley, J., Costa, C. G. S., Cowen, D. F., Dailing, J., Dalberg, E., De Young, T., Desiati, P., Dewulf, J. -P, Doksus, P., Edsjö, J., Ekström, P., Erlandsson, B., Feser, T., Gaug, M., Goldschmidt, A., Goobar, A., Gray, L., Haase, H., Hallgren, A., Halzen, F., Hanson, K., Hardtke, R., He, Y. D., Hellwig, M., Heukenkamp, H., Hill, G. C., Hulth, P. O., Hundertmark, S., Jacobsen, J., Kandhadai, V., Karle, A., Kim, J., Koci, B., Köpke, L., Kowalski, M., Leich, H., Leuthold, M., Lindahl, P., Liubarsky, I., Loaiza, P., Lowder, D. M., Ludvig, J., Madsen, J., Marciniewski, P., Matis, H. S., Mihalyi, A., Mikolajski, T., Miller, T. C., Minaeva, Y., Miočinović, P., Mock, P. C., Morse, R., Neunhöffer, T., Newcomer, F. M., Niessen, P., Nygren, D. R., Ogelman, H., Pérez De Los Heros, C., Porrata, R., Price, P. B., Rawlins, K., Reed, C., Rhode, W., Richards, A., Richter, S., Rodríguez Martino, J., Romenesko, P., Ross, D., Rubinstein, H., Sander, H. -G, Scheider, T., Schmidt, T., Schneider, D., Schneider, E., Schwarz, R., Silvestri, A., Solarz, M., Spiczak, G. M., Spiering, C., Starinsky, N., Steele, D., Steffen, P., Stokstad, R. G., Streicher, O., Sun, Q., Taboada, I., Thollander, L., Thon, T., Tilav, S., Usechak, N., Vander Donckt, M., Walck, C., Weinheimer, C., Wiebusch, C. H., Wischnewski, R., Wissing, H., Woschnagg, K., Wu, W., Yodh, G., and Young, S.
Abstract: We present results based on data taken in 1997 with the 302-PMT Antarctic Muon and Neutrino Detector Array-B10 ("AMANDA-B10") array. Atmospheric neutrinos created in the northern hemisphere are observed indirectly through their charged current interactions which produce relativistic, Cherenkov-light-emitting upgoing muons in the South Pole ice cap. The reconstructed angular distribution of these events is in good agreement with expectation and demonstrates the viability of this ice-based device as a neutrino telescope., Source: Scopus
Published: 2001
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4. Observation of high-energy neutrinos using Čerenkov detectors embedded deep in Antarctic ice

Author: Andrés, E., Askebjer, P., Bai, X., Barouch, G., Barwick, S. W., Bay, R. C., Becker, K. -H, Bergström, L., Bertrand, D., Bierenbaum, D., Biron, A., Booth, J., Botner, O., Bouchta, A., Boyce, M. M., Carius, Staffan, Chen, A., Chirkin, D., Conrad, J., Cooley, J., Costa, C. G. S., Cowen, D. F., Dailing, J., Dalberg, E., DeYoung, T., Desiati, P., Dewulf, J. -P, Doksus, P., Edsjö, J., Ekström, P., Erlandsson, B., Feser, T., Gaug, M., Goldschmidt, A., Goobar, A., Gray, L., Haase, H., Hallgren, A., Halzen, F., Hanson, K., Hardtke, R., He, Y. D., Hellwig, M., Heukenkamp, H., Hill, G. C., Hulth, P. O., Hundertmark, S., Jacobsen, J., Kandhadai, V., Karle, A., Kim, J., Koci, B., Köpke, L., Kowalski, M., Leich, H., Leuthold, M., Lindahl, P., Liubarsky, I., Loaiza, P., Lowder, D. M., Ludvig, J., Madsen, J., Marciniewski, P., Matis, H. S., Mihalyi, A., Mikolajski, T., Miller, T. C., Minaeva, Y., Miočinović, P., Mock, P. C., Morse, R., Neunhöffer, T., Newcomer, F. M., Niessen, P., Nygren, D. R., Ögelman, H., Pérez De Los Heros, C., Porrata, R., Price, P. B., Rawlins, K., Reed, C., Rhode, W., Richards, A., Richter, S., Martino, J. R., Romenesko, P., Ross, D., Rubinstein, H., Sander, H. -G, Scheider, T., Schmidt, T., Schneider, D., Schneider, E., Schwarz, R., Silvestri, A., Solarz, M., Spiczak, G. M., Spiering, C., Starinsky, N., Steele, D., Steffen, P., Stokstad, R. G., Streicher, O., Sun, Q., Taboada, I., Thollander, L., Thon, T., Tilav, S., Usechak, N., Vander Donckt, M., Walck, C., Weinheimer, C., Wiebusch, C. H., Wischnewski, R., Wissing, H., Woschnagg, K., Wu, W., Yodh, G., Young, S., Andrés, E., Askebjer, P., Bai, X., Barouch, G., Barwick, S. W., Bay, R. C., Becker, K. -H, Bergström, L., Bertrand, D., Bierenbaum, D., Biron, A., Booth, J., Botner, O., Bouchta, A., Boyce, M. M., Carius, Staffan, Chen, A., Chirkin, D., Conrad, J., Cooley, J., Costa, C. G. S., Cowen, D. F., Dailing, J., Dalberg, E., DeYoung, T., Desiati, P., Dewulf, J. -P, Doksus, P., Edsjö, J., Ekström, P., Erlandsson, B., Feser, T., Gaug, M., Goldschmidt, A., Goobar, A., Gray, L., Haase, H., Hallgren, A., Halzen, F., Hanson, K., Hardtke, R., He, Y. D., Hellwig, M., Heukenkamp, H., Hill, G. C., Hulth, P. O., Hundertmark, S., Jacobsen, J., Kandhadai, V., Karle, A., Kim, J., Koci, B., Köpke, L., Kowalski, M., Leich, H., Leuthold, M., Lindahl, P., Liubarsky, I., Loaiza, P., Lowder, D. M., Ludvig, J., Madsen, J., Marciniewski, P., Matis, H. S., Mihalyi, A., Mikolajski, T., Miller, T. C., Minaeva, Y., Miočinović, P., Mock, P. C., Morse, R., Neunhöffer, T., Newcomer, F. M., Niessen, P., Nygren, D. R., Ögelman, H., Pérez De Los Heros, C., Porrata, R., Price, P. B., Rawlins, K., Reed, C., Rhode, W., Richards, A., Richter, S., Martino, J. R., Romenesko, P., Ross, D., Rubinstein, H., Sander, H. -G, Scheider, T., Schmidt, T., Schneider, D., Schneider, E., Schwarz, R., Silvestri, A., Solarz, M., Spiczak, G. M., Spiering, C., Starinsky, N., Steele, D., Steffen, P., Stokstad, R. G., Streicher, O., Sun, Q., Taboada, I., Thollander, L., Thon, T., Tilav, S., Usechak, N., Vander Donckt, M., Walck, C., Weinheimer, C., Wiebusch, C. H., Wischnewski, R., Wissing, H., Woschnagg, K., Wu, W., Yodh, G., and Young, S.
Abstract: Neutrinos are elementary particles that carry no electric charge and have little mass. As they interact only weakly with other particles, they can penetrate enormous amounts of matter, and therefore have the potential to directly convey astrophysical information from the edge of the Universe and from deep inside the most cataclysmic high-energy regions. The neutrino's great penetrating power, however, also makes this particle difficult to detect. Underground detectors have observed low-energy neutrinos from the Sun and a nearby supernova2, as well as neutrinos generated in the Earth's atmosphere. But the very low fluxes of high-energy neutrinos from cosmic sources can be observed only by much larger, expandable detectors in, for example, deep water3,4 or ice5. Here we report the detection of upwardly propagating atmospheric neutrinos by the ice-based Antarctic muon and neutrino detector array (AMANDA). These results establish a technology with which to build a kilometre-scale neutrino observatory necessary for astrophysical observations1., Source: Scopus
Published: 2001
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5. Selected recent results from AMANDA

Author: Andres, E., Askebjer, P., Bai, X., Barouch, G., Barwick, S. W., Bay, R. C., Becker, K. H., Bergstrom, L., Bertrand, D., Bierenbaum, D., Biron, A., Booth, J., Botner, O., Bouchta, A., Boyce, M. M., Carius, Staffan, Chen, A., Chirkin, D., Conrad, J., Cooley, J., Costa, C. G. S., Cowen, D. F., Dailing, J., Dalberg, E., DeYoung, T., Desiati, P., Dewulf, J. P., Doksus, P., Edsjo, J., Ekstrom, P., Erlandsson, B., Feser, T., Gaug, M., Goldschmidt, A., Goobar, A., Gray, L., Haase, H., Hallgren, A., Halzen, F., Hanson, K., Hardtke, R., He, Y. D., Hellwig, M., Heukenkamp, H., Hill, G. C., Hulth, P. O., Hundertmark, S., Jacobsen, J., Kandhadai, V., Karle, A., Kim, J., Koci, B., Kopke, L., Kowalski, M., Leich, H., Leuthold, M., Lindahl, P., Liubarsky, I., Loaiza, P., Lowder, D. M., Ludvig, J., Madsen, J., Marciniewski, P., Matis, H. S., Mihalyi, A., Mikolajski, T., Miller, T. C., Minaeva, Y., Miocinovic, P., Mock, P. C., Morse, R., Neunhoffer, T., Newcomer, F. M., Niessen, P., Nygren, D. R., Ogelman, H., Peres de los Heros, C. P. D. L., Porrata, R., Price, P. B., Rawlins, K., Reed, C., Rhode, W., Richards, A., Richter, S., Martino, J. R., Romenesko, P., Ross, D., Rubinstein, H., Sander, H. G., Scheider, T., Schmidt, T., Schneider, D., Schneider, E., Schwarzl, R., Silvestri, A., Solarz, M., Spiczak, G. M., Spiering, C., Starinsky, N., Steele, D., Steffen, P., Stokstad, R. G., Streicher, O., Sun, A., Taboada, I., Thollander, L., Thon, T., Tilav, S., Usechak, N., Donckt, M. V., Walck, C., Weinheimer, C., Wiebusch, C. H., Wischnewski, R., Wissing, H., Woschnagg, K., Wu, W., Yodh, G., Young, S., Lim, C. S., Yamanaka, T., Andres, E., Askebjer, P., Bai, X., Barouch, G., Barwick, S. W., Bay, R. C., Becker, K. H., Bergstrom, L., Bertrand, D., Bierenbaum, D., Biron, A., Booth, J., Botner, O., Bouchta, A., Boyce, M. M., Carius, Staffan, Chen, A., Chirkin, D., Conrad, J., Cooley, J., Costa, C. G. S., Cowen, D. F., Dailing, J., Dalberg, E., DeYoung, T., Desiati, P., Dewulf, J. P., Doksus, P., Edsjo, J., Ekstrom, P., Erlandsson, B., Feser, T., Gaug, M., Goldschmidt, A., Goobar, A., Gray, L., Haase, H., Hallgren, A., Halzen, F., Hanson, K., Hardtke, R., He, Y. D., Hellwig, M., Heukenkamp, H., Hill, G. C., Hulth, P. O., Hundertmark, S., Jacobsen, J., Kandhadai, V., Karle, A., Kim, J., Koci, B., Kopke, L., Kowalski, M., Leich, H., Leuthold, M., Lindahl, P., Liubarsky, I., Loaiza, P., Lowder, D. M., Ludvig, J., Madsen, J., Marciniewski, P., Matis, H. S., Mihalyi, A., Mikolajski, T., Miller, T. C., Minaeva, Y., Miocinovic, P., Mock, P. C., Morse, R., Neunhoffer, T., Newcomer, F. M., Niessen, P., Nygren, D. R., Ogelman, H., Peres de los Heros, C. P. D. L., Porrata, R., Price, P. B., Rawlins, K., Reed, C., Rhode, W., Richards, A., Richter, S., Martino, J. R., Romenesko, P., Ross, D., Rubinstein, H., Sander, H. G., Scheider, T., Schmidt, T., Schneider, D., Schneider, E., Schwarzl, R., Silvestri, A., Solarz, M., Spiczak, G. M., Spiering, C., Starinsky, N., Steele, D., Steffen, P., Stokstad, R. G., Streicher, O., Sun, A., Taboada, I., Thollander, L., Thon, T., Tilav, S., Usechak, N., Donckt, M. V., Walck, C., Weinheimer, C., Wiebusch, C. H., Wischnewski, R., Wissing, H., Woschnagg, K., Wu, W., Yodh, G., Young, S., Lim, C. S., and Yamanaka, T.
Abstract: We present a selection of results based on data taken in 1997 with the 302-PMT Antarctic Muon and Neutrino Detector Array-B10 ("AMANDA-B10") array. Atmospheric neutrinos created in the northern hemisphere are observed indirectly through their charged current interactions which produce relativistic, Cherenkov-light-emitting upgoing muons in the South Pole ice cap. The reconstructed angular distribution of these events is in good agreement with expectation and demonstrates the viability of this ice-based device as a neutrino telescope. Studies of nearly vertical upgoing muons limit the available parameter space for WIMP dark matter under the assumption that WIMPS are trapped in the earth's gravitational potential well and annihilate with one another near the earth's center.
Published: 2001

6. WIMP searches with AMANDA-B10

Author: Edsjö, Joakim, Bai, X., Barouch, G., Barwick, S.W., Bay, R.C., Becker, K.-H., Bergström, L., Bertrand, D., Biron, A., Botner, O., Bouchta, A., Boyce, M.M., Carius, Staffan, Chen, A., Chirkin, D., Conrad, J., Cooley, J., Costa, C.G.S., Cowen, D.F., Dailing, J., Dalberg, E., Deyoung, T., Desiati, P., Dewulf, J.-P., Doksus, P., Ekström, P., Feser, T., Gaug, M., Goldschmidt, A., Goobar, A., Hallgren, A., Halzen, F., Hanson, K., Hardtke, R., Hellwig, M., Hill, G. C., Hulth, P.O., Hundertmark, S., Jacobsen, J., Karle, A., Kim, J ., Koci, B., Köpke, L., Kowalski, M., Lamoureux, J.I., Leich, H., Leuthold, M., Lindahl, P., Loaiza, P., Lowder, D.M., Ludvig, J., Madsen, J., Marcomoewski, P., Maris, H.S., Miller, T.C., Minaeva, Y., Miocinovic, P., Morse, R., Neunhöffer, T., Niessen, P., Nygren, D.R., Ogelman, H., Heros, C. Peres de Los, Price, P.B., Rawlins, K., Rhode, W., Richter, S., Martino, J. Rodriguez, Romenesko, P., Ross, D., Rubinstein, H., Sander, H.-G., Scheider, T., Schmidt, T., Schneider, D., Schwarz, R., Silvestri, A., Smoot, G., Solarz, M., Spiczak, G.M., Spiering, C., Starinsky, N., Steele, D., Steffen, P., Stokstad, R.G., Streicher, O., Taboada, I., Donckt, M. Vander, Walck, C., Weinheimer, C., Wiebusch, C.H., Wischnewski, R., Woschnagg, K., Wu, W., Yodh, G., Young, S., Edsjö, Joakim, Bai, X., Barouch, G., Barwick, S.W., Bay, R.C., Becker, K.-H., Bergström, L., Bertrand, D., Biron, A., Botner, O., Bouchta, A., Boyce, M.M., Carius, Staffan, Chen, A., Chirkin, D., Conrad, J., Cooley, J., Costa, C.G.S., Cowen, D.F., Dailing, J., Dalberg, E., Deyoung, T., Desiati, P., Dewulf, J.-P., Doksus, P., Ekström, P., Feser, T., Gaug, M., Goldschmidt, A., Goobar, A., Hallgren, A., Halzen, F., Hanson, K., Hardtke, R., Hellwig, M., Hill, G. C., Hulth, P.O., Hundertmark, S., Jacobsen, J., Karle, A., Kim, J ., Koci, B., Köpke, L., Kowalski, M., Lamoureux, J.I., Leich, H., Leuthold, M., Lindahl, P., Loaiza, P., Lowder, D.M., Ludvig, J., Madsen, J., Marcomoewski, P., Maris, H.S., Miller, T.C., Minaeva, Y., Miocinovic, P., Morse, R., Neunhöffer, T., Niessen, P., Nygren, D.R., Ogelman, H., Heros, C. Peres de Los, Price, P.B., Rawlins, K., Rhode, W., Richter, S., Martino, J. Rodriguez, Romenesko, P., Ross, D., Rubinstein, H., Sander, H.-G., Scheider, T., Schmidt, T., Schneider, D., Schwarz, R., Silvestri, A., Smoot, G., Solarz, M., Spiczak, G.M., Spiering, C., Starinsky, N., Steele, D., Steffen, P., Stokstad, R.G., Streicher, O., Taboada, I., Donckt, M. Vander, Walck, C., Weinheimer, C., Wiebusch, C.H., Wischnewski, R., Woschnagg, K., Wu, W., Yodh, G., and Young, S.
Abstract: 0
Published: 2001
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7. Status of the Neutrino Telescope AMANDA : Monopoles and WIMPS

Author: Bai, X., Barouch, G., Barwick, S. W., Bay, R. C., Becker, K. -H, Bergström, L., Bertrand, D., Biron, A., Botner, O., Bouchta, A., Boyce, M. M., Carius, Staffan, Chen, A., Chirkin, D., Conrad, J., Cooley, J., Costa, C. G. S., Cowen, D. F., Dailing, J., Dalberg, E., DeYoung, T., Desiati, P., Dewulf, J. -P, Doksus, P., Edsjö, J., Ekström, P., Feser, T., Gaug, M., Goldschmidt, A., Goobar, A., Hallgren, A., Halzen, F., Hanson, K., Hardtke, R., Hellwig, M., Hill, G. C., Hulth, P. O., Hundertmark, S., Jacobsen, J., Karle, A., Kim, J., Koci, B., Köpke, L., Kowalski, M., Lamoureux, J. I., Leich, H., Leuthold, M., Lindahl, P., Loaiza, P., Lowder, D. M., Ludvig, J., Madsen, J., Marciniewski, P., Matis, H. S., Miller, T. C., Minaeva, Y., Miočinović, P., Morse, R., Neunhöffer, T., Niessen, P., Nygren, D. R., Ogelman, H., Pérez de los Heros, C., Price, P. B., Rawlins, K., Rhode, W., Richter, S., Martino, J.Rodríguez, Romenesko, P., Ross, D., Rubinstein, H., Sander, H. -G, Scheider, T., Schmidt, T., Schneider, D., Schwarz, R., Silvestri, A., Smoot, G., Solarz, M., Spiczak, G. M., Spiering, C., Starinsky, N., Steele, D., Steffen, P., Stokstad, R. G., Streicher, O., Sudhoff, P., Taboada, I., Donckt, M., Walck, C., Weinheimer, C., Wiebusch, C. H., Wischnewski, R., Wissing, H., Woschnagg, K., Wu, W., Yodh, G., Young, S., Bai, X., Barouch, G., Barwick, S. W., Bay, R. C., Becker, K. -H, Bergström, L., Bertrand, D., Biron, A., Botner, O., Bouchta, A., Boyce, M. M., Carius, Staffan, Chen, A., Chirkin, D., Conrad, J., Cooley, J., Costa, C. G. S., Cowen, D. F., Dailing, J., Dalberg, E., DeYoung, T., Desiati, P., Dewulf, J. -P, Doksus, P., Edsjö, J., Ekström, P., Feser, T., Gaug, M., Goldschmidt, A., Goobar, A., Hallgren, A., Halzen, F., Hanson, K., Hardtke, R., Hellwig, M., Hill, G. C., Hulth, P. O., Hundertmark, S., Jacobsen, J., Karle, A., Kim, J., Koci, B., Köpke, L., Kowalski, M., Lamoureux, J. I., Leich, H., Leuthold, M., Lindahl, P., Loaiza, P., Lowder, D. M., Ludvig, J., Madsen, J., Marciniewski, P., Matis, H. S., Miller, T. C., Minaeva, Y., Miočinović, P., Morse, R., Neunhöffer, T., Niessen, P., Nygren, D. R., Ogelman, H., Pérez de los Heros, C., Price, P. B., Rawlins, K., Rhode, W., Richter, S., Martino, J.Rodríguez, Romenesko, P., Ross, D., Rubinstein, H., Sander, H. -G, Scheider, T., Schmidt, T., Schneider, D., Schwarz, R., Silvestri, A., Smoot, G., Solarz, M., Spiczak, G. M., Spiering, C., Starinsky, N., Steele, D., Steffen, P., Stokstad, R. G., Streicher, O., Sudhoff, P., Taboada, I., Donckt, M., Walck, C., Weinheimer, C., Wiebusch, C. H., Wischnewski, R., Wissing, H., Woschnagg, K., Wu, W., Yodh, G., and Young, S.
Abstract: The neutrino telescope AMANDA has been set up at the geographical South Pole as first step to a neutrino telescope of the scale of one cubic kilometer, which is the canonical size for a detector sensitive to neutrinos from Active Galactic Nuclei (AGN), Gamma Ray Bursts (GRB) and Topological Defects (TD). The location and depth in which the detector is installed is given by the requirement to detect neutrinos by the Cherenkov light produced by their reaction products and to keep the background due to atmospheric muons as small as possible. However, a detector optimized for this purpose is also capable to detect the bright Cherenkov light from relativistic Monopoles and neutrino signals from regions with high gravitational potential, where WIMPS are accumulated and possibly annihilate. Both hypothetical particles might contribute to the amount of dark matter. Therefore here a report about the status of the experiment (autumn 2000) and about the status of the search for these particles with the AMANDA B10 sub-detector is given.
Published: 2001
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8. Magnetic Fields in the Early Universe

Author: Grasso, Dario, Rubinstein, H. R., Grasso, Dario, and Rubinstein, H. R.
Abstract: This review concerns the origin and the possible effects of magnetic fields in the early Universe. We start by providing to the reader with a short overview of the current state of art of observations of cosmic magnetic fields. We then illustrate the arguments in favour of a primordial origin of magnetic fields in the galaxies and in the clusters of galaxies. We argue that the most promising way to test this hypothesis is to look for possible imprints of magnetic fields on the temperature and polarization anisotropies of the cosmic microwave background radiation (CMBR). With this purpose in mind, we provide a review of the most relevant effects of magnetic fields on the CMBR. A long chapter of this review is dedicated to particle physics inspired models which predict the generation of magnetic fields during the early Universe evolution. Although it is still unclear if any of these models can really explain the origin of galactic and intergalactic magnetic fields, we show that interesting effects may arise anyhow. Among these effects, we discuss the consequences of strong magnetic fields on the big-bang nucleosynthesis, on the masses and couplings of the matter constituents, on the electroweak phase transition, and on the baryon and lepton number violating sphaleron processes. Several intriguing common aspects, and possible interplay, of magnetogenesis and baryogenesis are also dicussed., Comment: 152 LaTeX pages, 6 figures., final version to appear in Phys. Rep
Published: 2000
Full Text: View/download PDF

9. Results from the AMANDA high energy neutrino detector

Author: Andres, E., Askebjer, P., Bai, X., Barouch, G., Barwick, S. W., Bay, R. C., Becker, K. -H, Bergström, L., Bertrand, D., Biron, A., Booth, J., Botner, O., Bouchta, A., Boyce, M. M., Carius, Staffan, Chirkin, D., Conrad, J., Costa, C. G. S., Cowen, D. F., Dailing, J., Dalberg, E., DeYoung, T., Desiati, P., Dewulf, J. -P, Doksus, P., Edsjö, J., Ekström, P., Erlandsson, B., Feser, T., Gaug, M., Goldschmidt, A., Goobar, A., Haase, H., Hallgren, A., Halzen, F., Hanson, K., Hardtke, R., He, Y. D., Hellwig, M., Heukenkamp, H., Hill, G. C., Hulth, P. O., Hundertmark, S., Jacobsen, J., Karle, A., Kim, J., Koci, B., Köpke, L., Kowalski, M., Leich, H., Leuthold, M., Lindahl, P., Liubarsky, I., Loaiza, P., Lowder, D. M., Ludvig, J., Madsen, J., Marciniewski, P., Matis, H., Mikolajski, T., Miller, T. C., Minaeva, Y., Miocinovic, P., Mock, P., Morse, R., Neunhöffer, T., Newcomer, F. M., Niessen, P., Nygren, D. R., Pérez de los Heros, C., Porrata, R., Price, P. B., Rawlins, K., Reed, C., Rhode, W., Richards, A., Richter, S., Rodriguez Martino, J., Romenesko, P., Ross, D., Rubinstein, H., Sander, H. -G, Scheider, T., Schmidt, T., Schneider, D., Schneider, E., Schwarz, R., Silvestri, A., Solarz, M., Spiczak, G., Spiering, C., Starinski, N., Steele, D., Steffen, P., Stokstad, R. G., Streicher, O., Sun, Q., Taboada, I., Thollander, L., Thon, T., Tilav, S., Vander Donckt, M., Walck, C., Weinheimer, C., Wiebusch, C. H., Wischnewski, R., Woschnagg, K., Wu, W., Yodh, G., Young, S., Andres, E., Askebjer, P., Bai, X., Barouch, G., Barwick, S. W., Bay, R. C., Becker, K. -H, Bergström, L., Bertrand, D., Biron, A., Booth, J., Botner, O., Bouchta, A., Boyce, M. M., Carius, Staffan, Chirkin, D., Conrad, J., Costa, C. G. S., Cowen, D. F., Dailing, J., Dalberg, E., DeYoung, T., Desiati, P., Dewulf, J. -P, Doksus, P., Edsjö, J., Ekström, P., Erlandsson, B., Feser, T., Gaug, M., Goldschmidt, A., Goobar, A., Haase, H., Hallgren, A., Halzen, F., Hanson, K., Hardtke, R., He, Y. D., Hellwig, M., Heukenkamp, H., Hill, G. C., Hulth, P. O., Hundertmark, S., Jacobsen, J., Karle, A., Kim, J., Koci, B., Köpke, L., Kowalski, M., Leich, H., Leuthold, M., Lindahl, P., Liubarsky, I., Loaiza, P., Lowder, D. M., Ludvig, J., Madsen, J., Marciniewski, P., Matis, H., Mikolajski, T., Miller, T. C., Minaeva, Y., Miocinovic, P., Mock, P., Morse, R., Neunhöffer, T., Newcomer, F. M., Niessen, P., Nygren, D. R., Pérez de los Heros, C., Porrata, R., Price, P. B., Rawlins, K., Reed, C., Rhode, W., Richards, A., Richter, S., Rodriguez Martino, J., Romenesko, P., Ross, D., Rubinstein, H., Sander, H. -G, Scheider, T., Schmidt, T., Schneider, D., Schneider, E., Schwarz, R., Silvestri, A., Solarz, M., Spiczak, G., Spiering, C., Starinski, N., Steele, D., Steffen, P., Stokstad, R. G., Streicher, O., Sun, Q., Taboada, I., Thollander, L., Thon, T., Tilav, S., Vander Donckt, M., Walck, C., Weinheimer, C., Wiebusch, C. H., Wischnewski, R., Woschnagg, K., Wu, W., Yodh, G., and Young, S.
Abstract: This paper briefly summarizes the search for astronomical sources of high-energy neutrinos using the AMANDA-B10 detector. The complete data set from 1997 was analyzed. For Eμ > 10 TeV, the detector exceeds 10,000 m2 in effective area between declinations of 25 and 90 degrees. Neutrinos generated in the atmosphere by cosmic ray interactions were used to verify the overall sensitivity of the detector. The absolute pointing accuracy and angular resolution has been confirmed by the analysis of coincident events between the SPASE air shower array and the AMANDA detector. Preliminary flux limits from point source candidates are presented. For declinations larger than +45 degrees, our results compare favorably to existing limits for sources in the Southern sky. We also present the current status of the searches for high energy neutrino emission from diffusely distributed sources, GRBs, and WIMPs from the center of the earth., Source: Scopus
Published: 2000
Full Text: View/download PDF

10. Magnetic Fields in the Early Universe

Author: Grasso, Dario, Rubinstein, H. R., Grasso, Dario, and Rubinstein, H. R.
Abstract: This review concerns the origin and the possible effects of magnetic fields in the early Universe. We start by providing to the reader with a short overview of the current state of art of observations of cosmic magnetic fields. We then illustrate the arguments in favour of a primordial origin of magnetic fields in the galaxies and in the clusters of galaxies. We argue that the most promising way to test this hypothesis is to look for possible imprints of magnetic fields on the temperature and polarization anisotropies of the cosmic microwave background radiation (CMBR). With this purpose in mind, we provide a review of the most relevant effects of magnetic fields on the CMBR. A long chapter of this review is dedicated to particle physics inspired models which predict the generation of magnetic fields during the early Universe evolution. Although it is still unclear if any of these models can really explain the origin of galactic and intergalactic magnetic fields, we show that interesting effects may arise anyhow. Among these effects, we discuss the consequences of strong magnetic fields on the big-bang nucleosynthesis, on the masses and couplings of the matter constituents, on the electroweak phase transition, and on the baryon and lepton number violating sphaleron processes. Several intriguing common aspects, and possible interplay, of magnetogenesis and baryogenesis are also dicussed., Comment: 152 LaTeX pages, 6 figures., final version to appear in Phys. Rep
Published: 2000
Full Text: View/download PDF

11. Magnetic Fields in the Early Universe

Author: Grasso, Dario, Rubinstein, H. R., Grasso, Dario, and Rubinstein, H. R.
Abstract: This review concerns the origin and the possible effects of magnetic fields in the early Universe. We start by providing to the reader with a short overview of the current state of art of observations of cosmic magnetic fields. We then illustrate the arguments in favour of a primordial origin of magnetic fields in the galaxies and in the clusters of galaxies. We argue that the most promising way to test this hypothesis is to look for possible imprints of magnetic fields on the temperature and polarization anisotropies of the cosmic microwave background radiation (CMBR). With this purpose in mind, we provide a review of the most relevant effects of magnetic fields on the CMBR. A long chapter of this review is dedicated to particle physics inspired models which predict the generation of magnetic fields during the early Universe evolution. Although it is still unclear if any of these models can really explain the origin of galactic and intergalactic magnetic fields, we show that interesting effects may arise anyhow. Among these effects, we discuss the consequences of strong magnetic fields on the big-bang nucleosynthesis, on the masses and couplings of the matter constituents, on the electroweak phase transition, and on the baryon and lepton number violating sphaleron processes. Several intriguing common aspects, and possible interplay, of magnetogenesis and baryogenesis are also dicussed., Comment: 152 LaTeX pages, 6 figures., final version to appear in Phys. Rep
Published: 2000
Full Text: View/download PDF

12. Magnetic Fields in the Early Universe

Author: Grasso, Dario, Rubinstein, H. R., Grasso, Dario, and Rubinstein, H. R.
Abstract: This review concerns the origin and the possible effects of magnetic fields in the early Universe. We start by providing to the reader with a short overview of the current state of art of observations of cosmic magnetic fields. We then illustrate the arguments in favour of a primordial origin of magnetic fields in the galaxies and in the clusters of galaxies. We argue that the most promising way to test this hypothesis is to look for possible imprints of magnetic fields on the temperature and polarization anisotropies of the cosmic microwave background radiation (CMBR). With this purpose in mind, we provide a review of the most relevant effects of magnetic fields on the CMBR. A long chapter of this review is dedicated to particle physics inspired models which predict the generation of magnetic fields during the early Universe evolution. Although it is still unclear if any of these models can really explain the origin of galactic and intergalactic magnetic fields, we show that interesting effects may arise anyhow. Among these effects, we discuss the consequences of strong magnetic fields on the big-bang nucleosynthesis, on the masses and couplings of the matter constituents, on the electroweak phase transition, and on the baryon and lepton number violating sphaleron processes. Several intriguing common aspects, and possible interplay, of magnetogenesis and baryogenesis are also dicussed., Comment: 152 LaTeX pages, 6 figures., final version to appear in Phys. Rep
Published: 2000
Full Text: View/download PDF

13. The AMANDA neutrino detector : Status report

Author: Wischnewski, R., Andrés, E., Bai, X., Barouch, G., Barwick, S., Bay, R., Becker, K., Bergström, L., Bertrand, D., Besson, D., Biron, A., Booth, J., Botner, O., Bouchta, A., Carius, Staffan, Carlson, M., Chinowsky, W., Chirkin, D., Conrad, J., Cowen, D. F., Costa, C., Dalberg, E., Desiati, P., Dewulf, J., Deyoung, T., Doksus, P., Edsjö, J., Ekström, P., Feser, T., Frichter, G., Gaisser, T., Goldschmidt, A., Goobar, A., Hallgren, A., Halzen, F., Hardtke, R., Hellwig, M., Hill, G., Hulth, P., Hundertmark, S., Jacobsen, J., Karle, A., Kim, J., Koepke, L., Kowalski, M., Kravchenko, I., Lamoureux, J., Leich, H., Leuthold, M., Lindahl, P., Liss, T., Loaiza, P., Lowder, D., Ludvig, J., Marciniewski, P., Matis, H., Miller, T., Miocinovic, P., Mock, P., Morse, R., Neunhoeffer, T., Newcomer, M., Niessen, P., Nygren, D., de los Heros, C. P., Porrata, R., Price, P., Przybylski, G., Rawlins, K., Rhode, W., Richter, S., Rodriguez, J., Romenesko, P., Ross, D., Rubinstein, H., Sander, H., Schäfer, U., Schmidt, T., Schneider, E., Schwarz, R., Schwendicke, U., Silvestri, A., Smoot, G., Solarz, M., Spiczak, G., Spiering, C., Starinski, N., Steffen, P., Stokstad, R., Streicher, O., Taboada, I., Thollander, L., Thon, T., Tilav, S., vander Donckt, M., Walck, C., Wiebusch, C., Woschnagg, K., Wu, W., Yodh, G., Young, S., Wischnewski, R., Andrés, E., Bai, X., Barouch, G., Barwick, S., Bay, R., Becker, K., Bergström, L., Bertrand, D., Besson, D., Biron, A., Booth, J., Botner, O., Bouchta, A., Carius, Staffan, Carlson, M., Chinowsky, W., Chirkin, D., Conrad, J., Cowen, D. F., Costa, C., Dalberg, E., Desiati, P., Dewulf, J., Deyoung, T., Doksus, P., Edsjö, J., Ekström, P., Feser, T., Frichter, G., Gaisser, T., Goldschmidt, A., Goobar, A., Hallgren, A., Halzen, F., Hardtke, R., Hellwig, M., Hill, G., Hulth, P., Hundertmark, S., Jacobsen, J., Karle, A., Kim, J., Koepke, L., Kowalski, M., Kravchenko, I., Lamoureux, J., Leich, H., Leuthold, M., Lindahl, P., Liss, T., Loaiza, P., Lowder, D., Ludvig, J., Marciniewski, P., Matis, H., Miller, T., Miocinovic, P., Mock, P., Morse, R., Neunhoeffer, T., Newcomer, M., Niessen, P., Nygren, D., de los Heros, C. P., Porrata, R., Price, P., Przybylski, G., Rawlins, K., Rhode, W., Richter, S., Rodriguez, J., Romenesko, P., Ross, D., Rubinstein, H., Sander, H., Schäfer, U., Schmidt, T., Schneider, E., Schwarz, R., Schwendicke, U., Silvestri, A., Smoot, G., Solarz, M., Spiczak, G., Spiering, C., Starinski, N., Steffen, P., Stokstad, R., Streicher, O., Taboada, I., Thollander, L., Thon, T., Tilav, S., vander Donckt, M., Walck, C., Wiebusch, C., Woschnagg, K., Wu, W., Yodh, G., and Young, S.
Abstract: The first stage of the AMANDA High Energy Neutrino Detector at the South Pole, the 302 PMT array AMANDA-B10, is taking data since 1997. We describe results on atmospheric neutrinos, limits on indirect WIMP detection, seasonal muon flux variation, relativistic monopole flux limits, a search for gravitational collapse neutrinos, and a depth scan of the optical ice properties. The next stage 19-string detector AMANDA-II with ∼650 PMTs will be completed in spring 2000., Source: Scopus
Published: 2000
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14. The AMANDA neutrino telescope : Principle of operation and first results

Author: Andres, E., Askebjer, P., Barwick, S. W., Bay, R., Bergström, L., Biron, A., Booth, J., Bouchta, A., Carius, Staffan, Carlson, M., Cowen, D., Dalberg, E., Deyoung, T., Ekström, P., Erlandson, B., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Hardtke, R., Hart, S., He, Y., Heukenkamp, H., Hill, G., Hulth, P. O., Hundertmark, S., Jacobsen, J., Jones, A., Kandhadai, V., Karle, A., Koci, B., Lindahl, P., Liubarsky, I., Leuthold, M., Lowder, D. M., Marciniewski, P., Mikolajski, T., Miller, T., Miocinovic, P., Mock, P., Morse, R., Niessen, P., Pérez De Los Heros, C., Porrata, R., Potter, D., Price, P. B., Przybylski, G., Richards, A., Richter, S., Romenesko, P., Rubinstein, H., Schneider, E., Schmidt, T., Schwarz, R., Solarz, M., Spiczak, G. M., Spiering, C., Streicher, O., Sun, Q., Thollander, L., Thon, T., Tilav, S., Walck, C., Wiebusch, C., Wischnewski, R., Woschnagg, K., Yodh, G., Andres, E., Askebjer, P., Barwick, S. W., Bay, R., Bergström, L., Biron, A., Booth, J., Bouchta, A., Carius, Staffan, Carlson, M., Cowen, D., Dalberg, E., Deyoung, T., Ekström, P., Erlandson, B., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Hardtke, R., Hart, S., He, Y., Heukenkamp, H., Hill, G., Hulth, P. O., Hundertmark, S., Jacobsen, J., Jones, A., Kandhadai, V., Karle, A., Koci, B., Lindahl, P., Liubarsky, I., Leuthold, M., Lowder, D. M., Marciniewski, P., Mikolajski, T., Miller, T., Miocinovic, P., Mock, P., Morse, R., Niessen, P., Pérez De Los Heros, C., Porrata, R., Potter, D., Price, P. B., Przybylski, G., Richards, A., Richter, S., Romenesko, P., Rubinstein, H., Schneider, E., Schmidt, T., Schwarz, R., Solarz, M., Spiczak, G. M., Spiering, C., Streicher, O., Sun, Q., Thollander, L., Thon, T., Tilav, S., Walck, C., Wiebusch, C., Wischnewski, R., Woschnagg, K., and Yodh, G.
Abstract: AMANDA is a high-energy neutrino telescope presently under construction at the geographical South Pole. In the Antarctic summer 1995/96, an array of 80 optical modules (OMs) arranged on 4 strings (AMANDA-B4) was deployed at depths between 1.5 and 2 km. In this paper we describe the design and performance of the AMANDA-B4 prototype, based on data collected between February and November 1996. Monte Carlo simulations of the detector response to down-going atmospheric muon tracks show that the global behavior of the detector is understood. We describe the data analysis method and present first results on atmospheric muon reconstruction and separation of neutrino candidates. The AMANDA array was upgraded with 216 OMs on 6 new strings in 1996/97 (AMANDA-B10), and 122 additional OMs on 3 strings in 1997/98., Source: Scopus
Published: 2000
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15. Observation of high energy atmospheric neutrinos with AMANDA

Author: Karle, A., Andres, E., Askebjer, P., Bai, X., Barouch, G., Barwick, S. W., Bay, R. C., Becker, K. -H, Bergstrom, L., Bertrand, D., Bierenbaum, D., Biron, A., Booth, J., Botner, O., Bouchta, A., Boyce, M. M., Carius, Staffan, Chen, A., Chirkin, D., Conard, J., Cooley, J., Costa, C. G. S., Cowen, D. F., Dailing, J., Dalberg, E., DeYoung, T., Desiati, P., Dewulf, J. -P, Dokus, P., Edsjo, J., Ekstrom, P., Erlandsson, B., Feser, T., Gaug, M., Goldschmidt, A., Goobar, A., Gray, L., Haase, H., Hallgren, A., Halzen, F., Hanson, K., Hardtke, R., He, Y. D., Hellwig, M., Heukenkamp, H., Hill, G. C., Hulth, P. O., Hundertmark, S., Jacobsen, J., Kandhadai, V., Kim, J., Koci, B., Kopke, L., Kowalski, M., Leich, H., Leuthold, M., Lindahl, P., Liubarsky, I., Loaiza, P., Lowder, D. M., Ludvig, J., Madsen, J., Marciniewski, P., Matis, H. S., Mihalyi, A., Mikolajski, T., Miller, T. C., Minaeva, Y., Miocinovic, P., Mock, P. C., Morse, R., Neunhoffer, T., Newcomer, F. M., Niessen, P., Nygren, D. R., Ogelman, H., Perez de los Heros, C., Porrata, R., Price, P. B., Rawlins, K., Reed, C., Rhode, W., Richards, A., Richter, S., Martino, J. R., Romenesko, P., Ross, D., Rubinstein, H., Sander, H. -G, Scheider, T., Schmidt, T., Schneider, D., Schneider, E., Schwarz, R., Silvestri, A., Solarz, M., Spiczak, G., Spiering, C., Starinsky, N., Steele, D., Steffen, P., Stokstad, R. G., Streicher, O., Sun, Q., Taboada, I., Thollander, L., Thon, T., Tilav, S., Usechak, N., Donckt, M. V., Walck, C., Weinheimer, C., Wiebusch, C. H., Wischnewski, R., Woschnagg, K., Wu, W., Yodh, G., Young, S., Karle, A., Andres, E., Askebjer, P., Bai, X., Barouch, G., Barwick, S. W., Bay, R. C., Becker, K. -H, Bergstrom, L., Bertrand, D., Bierenbaum, D., Biron, A., Booth, J., Botner, O., Bouchta, A., Boyce, M. M., Carius, Staffan, Chen, A., Chirkin, D., Conard, J., Cooley, J., Costa, C. G. S., Cowen, D. F., Dailing, J., Dalberg, E., DeYoung, T., Desiati, P., Dewulf, J. -P, Dokus, P., Edsjo, J., Ekstrom, P., Erlandsson, B., Feser, T., Gaug, M., Goldschmidt, A., Goobar, A., Gray, L., Haase, H., Hallgren, A., Halzen, F., Hanson, K., Hardtke, R., He, Y. D., Hellwig, M., Heukenkamp, H., Hill, G. C., Hulth, P. O., Hundertmark, S., Jacobsen, J., Kandhadai, V., Kim, J., Koci, B., Kopke, L., Kowalski, M., Leich, H., Leuthold, M., Lindahl, P., Liubarsky, I., Loaiza, P., Lowder, D. M., Ludvig, J., Madsen, J., Marciniewski, P., Matis, H. S., Mihalyi, A., Mikolajski, T., Miller, T. C., Minaeva, Y., Miocinovic, P., Mock, P. C., Morse, R., Neunhoffer, T., Newcomer, F. M., Niessen, P., Nygren, D. R., Ogelman, H., Perez de los Heros, C., Porrata, R., Price, P. B., Rawlins, K., Reed, C., Rhode, W., Richards, A., Richter, S., Martino, J. R., Romenesko, P., Ross, D., Rubinstein, H., Sander, H. -G, Scheider, T., Schmidt, T., Schneider, D., Schneider, E., Schwarz, R., Silvestri, A., Solarz, M., Spiczak, G., Spiering, C., Starinsky, N., Steele, D., Steffen, P., Stokstad, R. G., Streicher, O., Sun, Q., Taboada, I., Thollander, L., Thon, T., Tilav, S., Usechak, N., Donckt, M. V., Walck, C., Weinheimer, C., Wiebusch, C. H., Wischnewski, R., Woschnagg, K., Wu, W., Yodh, G., and Young, S.
Abstract: In 1997 the Antarctic Muon and Neutrino Detector Array (AMANDA) started operating with 10 strings. In an analysis of data taken during the first year of operation 188 atmospheric neutrino candidates were found. Their zenith angle distribution agrees with expectations based on Monte Carlo simulations. A preliminary upper limit is given on a diffuse flux of high energy neutrinos of astrophysical origin.
Published: 2000

16. Constraints on the Variation of the Fine Structure Constant from Big Bang Nucleosynthesis

Author: Bergstrom, L., Iguri, S., Rubinstein, H., Bergstrom, L., Iguri, S., and Rubinstein, H.
Abstract: We put bounds on the variation of the value of the fine structure constant $\alpha$, at the time of Big Bang nucleosynthesis. We study carefully all light elements up to $^7$Li. We correct a previous upper limit on $|\Delta \alpha / \alpha|$ estimated from $^4$He primordial abundance and we find interesting new potential limits (depending on the value of the baryon-to-photon ratio) from $^7$Li, whose production is governed to a large extent by Coulomb barriers. The presently unclear observational situation concerning the primordial abundances preclude a better limit than $|\Delta \alpha/\alpha| \lsim 2\cdot 10^{-2}$, two orders of magnitude less restrictive than previous bounds. In fact, each of the (mutually exclusive) scenarios of standard Big Bang nucleosynthesis proposed, one based on a high value of the measured deuterium primordial abundance and one based on a low value, may describe some aspects of data better if a change in $\alpha$ of this magnitude is assumed., Comment: 21 pages, eps figures embedded using epsfig macro
Published: 1999
Full Text: View/download PDF

17. Constraints on the Variation of the Fine Structure Constant from Big Bang Nucleosynthesis

Author: Bergstrom, L., Iguri, S., Rubinstein, H., Bergstrom, L., Iguri, S., and Rubinstein, H.
Abstract: We put bounds on the variation of the value of the fine structure constant $\alpha$, at the time of Big Bang nucleosynthesis. We study carefully all light elements up to $^7$Li. We correct a previous upper limit on $|\Delta \alpha / \alpha|$ estimated from $^4$He primordial abundance and we find interesting new potential limits (depending on the value of the baryon-to-photon ratio) from $^7$Li, whose production is governed to a large extent by Coulomb barriers. The presently unclear observational situation concerning the primordial abundances preclude a better limit than $|\Delta \alpha/\alpha| \lsim 2\cdot 10^{-2}$, two orders of magnitude less restrictive than previous bounds. In fact, each of the (mutually exclusive) scenarios of standard Big Bang nucleosynthesis proposed, one based on a high value of the measured deuterium primordial abundance and one based on a low value, may describe some aspects of data better if a change in $\alpha$ of this magnitude is assumed., Comment: 21 pages, eps figures embedded using epsfig macro
Published: 1999
Full Text: View/download PDF

18. Constraints on the Variation of the Fine Structure Constant from Big Bang Nucleosynthesis

Author: Bergstrom, L., Iguri, S., Rubinstein, H., Bergstrom, L., Iguri, S., and Rubinstein, H.
Abstract: We put bounds on the variation of the value of the fine structure constant $\alpha$, at the time of Big Bang nucleosynthesis. We study carefully all light elements up to $^7$Li. We correct a previous upper limit on $|\Delta \alpha / \alpha|$ estimated from $^4$He primordial abundance and we find interesting new potential limits (depending on the value of the baryon-to-photon ratio) from $^7$Li, whose production is governed to a large extent by Coulomb barriers. The presently unclear observational situation concerning the primordial abundances preclude a better limit than $|\Delta \alpha/\alpha| \lsim 2\cdot 10^{-2}$, two orders of magnitude less restrictive than previous bounds. In fact, each of the (mutually exclusive) scenarios of standard Big Bang nucleosynthesis proposed, one based on a high value of the measured deuterium primordial abundance and one based on a low value, may describe some aspects of data better if a change in $\alpha$ of this magnitude is assumed., Comment: 21 pages, eps figures embedded using epsfig macro
Published: 1999
Full Text: View/download PDF

19. Constraints on the Variation of the Fine Structure Constant from Big Bang Nucleosynthesis

Author: Bergstrom, L., Iguri, S., Rubinstein, H., Bergstrom, L., Iguri, S., and Rubinstein, H.
Abstract: We put bounds on the variation of the value of the fine structure constant $\alpha$, at the time of Big Bang nucleosynthesis. We study carefully all light elements up to $^7$Li. We correct a previous upper limit on $|\Delta \alpha / \alpha|$ estimated from $^4$He primordial abundance and we find interesting new potential limits (depending on the value of the baryon-to-photon ratio) from $^7$Li, whose production is governed to a large extent by Coulomb barriers. The presently unclear observational situation concerning the primordial abundances preclude a better limit than $|\Delta \alpha/\alpha| \lsim 2\cdot 10^{-2}$, two orders of magnitude less restrictive than previous bounds. In fact, each of the (mutually exclusive) scenarios of standard Big Bang nucleosynthesis proposed, one based on a high value of the measured deuterium primordial abundance and one based on a low value, may describe some aspects of data better if a change in $\alpha$ of this magnitude is assumed., Comment: 21 pages, eps figures embedded using epsfig macro
Published: 1999
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20. Status of the AMANDA experiment

Author: Andrés, E., Askebjer, P., Barwick, S. W., Bay, R., Bergström, L., Bouchta, A., Biron, A., Carius, Staffan, Costa, C., Cowen, D., Dalberg, E., Ekström, P., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Hart, S., He, Y., Hill, G., Hulth, P. O., Hundertmark, S., Jacobsen, J., Jones, A., Kandahai, V., Karle, A., Lindahl, P., Liubarsky, I., Lowder, D. M., Marciniewski, P., Mikolajski, T., Miller, T., Mock, P., Morse, R., Niessen, P., Nygren, D., Perez de Los Heros, C., Porrata, R., Potter, D., Price, P. B., Richards, A., Rubinstein, H., Schneider, E., Schwarz, R., Spiering, C., Streicher, O., Thon, T., Tilav, S., Walck, C., Wiebusch, C., Wischnewski, R., Woschnagg, K., Yodh, G., Andrés, E., Askebjer, P., Barwick, S. W., Bay, R., Bergström, L., Bouchta, A., Biron, A., Carius, Staffan, Costa, C., Cowen, D., Dalberg, E., Ekström, P., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Hart, S., He, Y., Hill, G., Hulth, P. O., Hundertmark, S., Jacobsen, J., Jones, A., Kandahai, V., Karle, A., Lindahl, P., Liubarsky, I., Lowder, D. M., Marciniewski, P., Mikolajski, T., Miller, T., Mock, P., Morse, R., Niessen, P., Nygren, D., Perez de Los Heros, C., Porrata, R., Potter, D., Price, P. B., Richards, A., Rubinstein, H., Schneider, E., Schwarz, R., Spiering, C., Streicher, O., Thon, T., Tilav, S., Walck, C., Wiebusch, C., Wischnewski, R., Woschnagg, K., and Yodh, G.
Abstract: The AMANDA high energy neutrino telescope has successfully been increased in size from four detector strings to ten detector strings during the 1996/1997 season. The first upward going muon-neutrino candidates have been reconstructed from the 1996 year's four-string data. Three new detector strings will be deployed during 1997/1998 to 2350 metres depth., Source: Scopus
Published: 1999
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21. The AMANDA neutrino telescope

Author: Andrés, E. C., Askebjer, P., Barwick, S. W., Bay, R. C., Bergström, L., Biron, A., Booth, J., Botner, O., Bouchta, A., Carius, Staffan, Carlson, M., Chinowsky, W., Chirkin, D., Conrad, J., Costa, C. G. S., Cowen, D., Dalberg, E., DeYoung, T., Edsjö, J., Ekström, P., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Hardtke, R., Hart, S., He, Y., De Los Heros, C. P., Hill, G., Hulth, P. O., Hundertmark, S., Jacobsen, J., Jones, A., Kandhadai, V., Karle, A., Kim, J., Leich, H., Leuthold, M., Lindahl, P., Liubarsky, I., Loaiza, P., Lowder, D., Marciniewski, P., Miller, T. C., Miocinovic, P., Mock, P. C., Morse, R., Newcomer, M., Niessen, P., Nygren, D., Porrata, R., Potter, D., Price, P. B., Przybylski, G., Rhode, W., Richter, S., Rodriguez, J., Romenesko, P., Ross, D., Rubinstein, H., Schmidt, T., Schneider, E., Schwarz, R., Schwendicke, U., Smoot, G., Solarz, M., Sorin, V., Spiering, C., Steffen, P., Stokstad, R., Streicher, O., Taboada, I., Thon, T., Tilav, S., Walck, C., Wiebusch, C. H., Wischnewski, R., Woschnagg, K., Wu, W., Yodh, G., Young, S., Andrés, E. C., Askebjer, P., Barwick, S. W., Bay, R. C., Bergström, L., Biron, A., Booth, J., Botner, O., Bouchta, A., Carius, Staffan, Carlson, M., Chinowsky, W., Chirkin, D., Conrad, J., Costa, C. G. S., Cowen, D., Dalberg, E., DeYoung, T., Edsjö, J., Ekström, P., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Hardtke, R., Hart, S., He, Y., De Los Heros, C. P., Hill, G., Hulth, P. O., Hundertmark, S., Jacobsen, J., Jones, A., Kandhadai, V., Karle, A., Kim, J., Leich, H., Leuthold, M., Lindahl, P., Liubarsky, I., Loaiza, P., Lowder, D., Marciniewski, P., Miller, T. C., Miocinovic, P., Mock, P. C., Morse, R., Newcomer, M., Niessen, P., Nygren, D., Porrata, R., Potter, D., Price, P. B., Przybylski, G., Rhode, W., Richter, S., Rodriguez, J., Romenesko, P., Ross, D., Rubinstein, H., Schmidt, T., Schneider, E., Schwarz, R., Schwendicke, U., Smoot, G., Solarz, M., Sorin, V., Spiering, C., Steffen, P., Stokstad, R., Streicher, O., Taboada, I., Thon, T., Tilav, S., Walck, C., Wiebusch, C. H., Wischnewski, R., Woschnagg, K., Wu, W., Yodh, G., and Young, S.
Abstract: With an effective telescope area of order 104 m2 for TeV neutrinos, a threshold near ∼50 GeV and a pointing accuracy of 2.5 degrees per muon track, the AMANDA detector represents the first of a new generation of high energy neutrino telescopes, reaching a scale envisaged over 25 years ago. We describe early results on the calibration of natural deep ice as a particle detector as well as on AMANDA's performance as a neutrino telescope., Source: Scopus
Published: 1999
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22. The AMANDA neutrino detector

Author: Wischnewski, R., Andrés, E., Askebjer, P., Barwick, S., Bay, R., Bergström, L., Biron, A., Booth, J., Botner, O., Bouchta, A., Carius, Staffan, Carlson, M., Chinowsky, W., Chirkin, D., Cowen, D., Costa, C., Dalberg, E., Deyoung, T., Edsjo, J., Ekström, P., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Hardtke, R., He, Y., Hill, G., Hulth, P., Hundertmark, S., Jacobsen, J., Kandhadai, V., Karle, A., Kim, J., Leich, H., Leuthold, M., Lindahl, P., Liss, T., Liubarsky, I., Loaiza, P., Lowder, D., Marciniewski, P., Miller, T., Miocinovic, P., Mock, P., Morse, R., Newcomer, M., Niessen, P., Nygren, D., Pérez de los Hcros, C., Porrata, R., Price, P., Przybylski, G., Rhode, W., Richter, S., Rodriguez, J., Romenesko, P., Ross, D., Rubinstein, H., Schmidt, T., Schneider, E., Schwarz, R., Schwendicke, U., Smoot, G., Solarz, M., Sorin, V., Spiering, C., Steffen, P., Stokstad, R., Streicher, O., Thollander, L., Thon, T., Tilav, S., Walck, C., Wiebusch, C., Woschnagg, K., Wu, W., Yodh, G., Young, S., Wischnewski, R., Andrés, E., Askebjer, P., Barwick, S., Bay, R., Bergström, L., Biron, A., Booth, J., Botner, O., Bouchta, A., Carius, Staffan, Carlson, M., Chinowsky, W., Chirkin, D., Cowen, D., Costa, C., Dalberg, E., Deyoung, T., Edsjo, J., Ekström, P., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Hardtke, R., He, Y., Hill, G., Hulth, P., Hundertmark, S., Jacobsen, J., Kandhadai, V., Karle, A., Kim, J., Leich, H., Leuthold, M., Lindahl, P., Liss, T., Liubarsky, I., Loaiza, P., Lowder, D., Marciniewski, P., Miller, T., Miocinovic, P., Mock, P., Morse, R., Newcomer, M., Niessen, P., Nygren, D., Pérez de los Hcros, C., Porrata, R., Price, P., Przybylski, G., Rhode, W., Richter, S., Rodriguez, J., Romenesko, P., Ross, D., Rubinstein, H., Schmidt, T., Schneider, E., Schwarz, R., Schwendicke, U., Smoot, G., Solarz, M., Sorin, V., Spiering, C., Steffen, P., Stokstad, R., Streicher, O., Thollander, L., Thon, T., Tilav, S., Walck, C., Wiebusch, C., Woschnagg, K., Wu, W., Yodh, G., and Young, S.
Abstract: The first stage of the AMANDA High Energy Neutrino Detector at the South Pole, the 302 PMT array AMANDA-B with an expected effective area for TeV neutrinos of ∼ 104 m2, has been taking data since 1997. Progress with calibration, investigation of ice properties, as well as muon and neutrino data analysis are described. The next stage 20-string detector AMANDA-II with ∼800 PMTs will be completed in spring 2000., Source: Scopus
Published: 1999
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23. Investigation of the Critical Behavior of the Critical Point of the Z2 Gauge Lattice

Author: Blum, Y., Coyle, P. K., Elitzur, S., Rabinovici, E., Solomon, S., Rubinstein, H., Blum, Y., Coyle, P. K., Elitzur, S., Rabinovici, E., Solomon, S., and Rubinstein, H.
Abstract: We investigate, through Monte-Carlo simulations, the nature of the second order point in a $Z_2$ (Bosonic) + $Z_2$ gauge theory in four dimensions. Detailed analysis of the critical exponents point to the Ising universality class. Relevancy to extended models and possible Non-Gaussian behavior is discussed., Comment: 4 pages, 6 figures, LaTex
Published: 1998
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24. Investigation of the Critical Behavior of the Critical Point of the Z2 Gauge Lattice

Author: Blum, Y., Coyle, P. K., Elitzur, S., Rabinovici, E., Solomon, S., Rubinstein, H., Blum, Y., Coyle, P. K., Elitzur, S., Rabinovici, E., Solomon, S., and Rubinstein, H.
Abstract: We investigate, through Monte-Carlo simulations, the nature of the second order point in a $Z_2$ (Bosonic) + $Z_2$ gauge theory in four dimensions. Detailed analysis of the critical exponents point to the Ising universality class. Relevancy to extended models and possible Non-Gaussian behavior is discussed., Comment: 4 pages, 6 figures, LaTex
Published: 1998
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25. Investigation of the Critical Behavior of the Critical Point of the Z2 Gauge Lattice

Author: Blum, Y., Coyle, P. K., Elitzur, S., Rabinovici, E., Solomon, S., Rubinstein, H., Blum, Y., Coyle, P. K., Elitzur, S., Rabinovici, E., Solomon, S., and Rubinstein, H.
Abstract: We investigate, through Monte-Carlo simulations, the nature of the second order point in a $Z_2$ (Bosonic) + $Z_2$ gauge theory in four dimensions. Detailed analysis of the critical exponents point to the Ising universality class. Relevancy to extended models and possible Non-Gaussian behavior is discussed., Comment: 4 pages, 6 figures, LaTex
Published: 1998
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26. The AMANDA neutrino telescope and the indirect search for dark matter : AMANDA Colaboration

Author: Bay, R. C., He, Y., Lowder, D., Miocinovic, P., Price, P. B., Solarz, M., Woschnagg, K., Barwick, S. W., Booth, J., Mock, P. C., Porrata, R., Schneider, E., Yodh, G., Cowen, D., Carlson, M., Costa, C. G. S., Deyoung, T., Gray, L., Halzen, F., Hardtke, R., Jacobsen, J., Kankhadai, V., Karle, A., Liubarsky, I., Morse, R., Tilav, S., Miller, T. C., Andrés, E. C., Askebjer, P., Bergström, L., Bouchta, A., Dalberg, E., Ekström, P., Goobar, A., Hulth, P. O., Walck, C., Hallgren, A., Heros, C. P. D. L., Marciniewski, P., Rubinstein, H., Carius, Staffan, Lindahl, P., Biron, A., Hundertmark, S., Leuthold, M., Niessen, P., Spiering, C., Streicher, O., Thon, T., Wiebusch, C. H., Wischnewski, R., Nygren, D., Jones, A., Hart, S., Potter, D., Hill, G., Schwarz, R., Bay, R. C., He, Y., Lowder, D., Miocinovic, P., Price, P. B., Solarz, M., Woschnagg, K., Barwick, S. W., Booth, J., Mock, P. C., Porrata, R., Schneider, E., Yodh, G., Cowen, D., Carlson, M., Costa, C. G. S., Deyoung, T., Gray, L., Halzen, F., Hardtke, R., Jacobsen, J., Kankhadai, V., Karle, A., Liubarsky, I., Morse, R., Tilav, S., Miller, T. C., Andrés, E. C., Askebjer, P., Bergström, L., Bouchta, A., Dalberg, E., Ekström, P., Goobar, A., Hulth, P. O., Walck, C., Hallgren, A., Heros, C. P. D. L., Marciniewski, P., Rubinstein, H., Carius, Staffan, Lindahl, P., Biron, A., Hundertmark, S., Leuthold, M., Niessen, P., Spiering, C., Streicher, O., Thon, T., Wiebusch, C. H., Wischnewski, R., Nygren, D., Jones, A., Hart, S., Potter, D., Hill, G., and Schwarz, R.
Abstract: With an effective telescope area of order 104m2, a threshold of ~50GeV and a pointing accuracy of 2.5°, the AMANDA detector represents the first of a new generation of high energy neutrino telescopes, reaching a scale envisaged over 25 years ago. We describe its performance, focussing on the capability to detect halo dark matter particles via their annihilation into neutrinos., Source: Scopus
Published: 1998
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27. Initial results from the AMANDA high-energy neutrino detector

Author: Barwick, S. W., Booth, J., Kim, J., Mock, R., Porrata, R., Ross, D., Wu, W., Yodh, G., Young, S., Miller, T., Biron, A., Hundertmark, S., Leich, H., Leothold, M., Niessen, P., Richter, S., Schmidt, T., Schwendicke, U., Spiering, C., Steffen, P., Streicher, O., Thon, T., Wiebusch, C., Wischnewski, R., Carius, Staffan, Lindahl, P., Andres, E., Bergstrom, L., Bouchta, A., Dalberg, E., Edsjo, J., Ekstrom, P., Goodbar, A., Hulth, P., Rodriguez, J., Walck, C., Bay, R., He, Y., Lowder, D., Miocinovic, P., Price, P. B., Rhode, W., Solarz, M., Woschnagg, K., Cowen, D., Newcomer, M., Carlson, M., DeYoung, T., Halzen, F., Hardtke, R., Hill, G., Jacobsen, J., Kandhadai, V., Karle, A., Liubarsky, I., Morse, R., Romenesko, P., Tilav, S., Chinowsky, W., Nygren, D., Przybylski, G., Smoot, George F., Stokstad, R., Botner, O., Hallgren, A., Loaiza, P., Marciniewski, P., Perez de los Heros, C., Rubinstein, H., Barwick, S. W., Booth, J., Kim, J., Mock, R., Porrata, R., Ross, D., Wu, W., Yodh, G., Young, S., Miller, T., Biron, A., Hundertmark, S., Leich, H., Leothold, M., Niessen, P., Richter, S., Schmidt, T., Schwendicke, U., Spiering, C., Steffen, P., Streicher, O., Thon, T., Wiebusch, C., Wischnewski, R., Carius, Staffan, Lindahl, P., Andres, E., Bergstrom, L., Bouchta, A., Dalberg, E., Edsjo, J., Ekstrom, P., Goodbar, A., Hulth, P., Rodriguez, J., Walck, C., Bay, R., He, Y., Lowder, D., Miocinovic, P., Price, P. B., Rhode, W., Solarz, M., Woschnagg, K., Cowen, D., Newcomer, M., Carlson, M., DeYoung, T., Halzen, F., Hardtke, R., Hill, G., Jacobsen, J., Kandhadai, V., Karle, A., Liubarsky, I., Morse, R., Romenesko, P., Tilav, S., Chinowsky, W., Nygren, D., Przybylski, G., Smoot, George F., Stokstad, R., Botner, O., Hallgren, A., Loaiza, P., Marciniewski, P., Perez de los Heros, C., and Rubinstein, H.
Published: 1998

28. 50 TeV HEGRA Sources and Infrared Radiation

Author: Berezinsky, V., Bergström, Lars, Rubinstein, H. R., Berezinsky, V., Bergström, Lars, and Rubinstein, H. R.
Abstract: The recent observations of 50 TeV gamma radiation by HEGRA have the potential of determining the extragalactic flux of infrared radiation. The fact that radiation is observed in the range between 30 and 100 TeV sets an upper limit on the infrared flux, while a cutoff at $E_{\gamma} \approx 50$ TeV fixes this flux with a good accuracy. If the intrinsic radiation is produced due to interaction of high energy protons with gas or low-energy target photons, then an accompaning high-energy neutrino flux is unavoidable. We calculate this flux and underground muon flux produced by it. The muon flux is dominated by muons with energies about 1 TeV and can be marginally detected by a 1 km$^2$ detector like an expanded AMANDA., Comment: 9 pages, latex2e, 3 eps figures
Published: 1997
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29. 50 TeV HEGRA Sources and Infrared Radiation

Author: Berezinsky, V., Bergström, Lars, Rubinstein, H. R., Berezinsky, V., Bergström, Lars, and Rubinstein, H. R.
Abstract: The recent observations of 50 TeV gamma radiation by HEGRA have the potential of determining the extragalactic flux of infrared radiation. The fact that radiation is observed in the range between 30 and 100 TeV sets an upper limit on the infrared flux, while a cutoff at $E_{\gamma} \approx 50$ TeV fixes this flux with a good accuracy. If the intrinsic radiation is produced due to interaction of high energy protons with gas or low-energy target photons, then an accompaning high-energy neutrino flux is unavoidable. We calculate this flux and underground muon flux produced by it. The muon flux is dominated by muons with energies about 1 TeV and can be marginally detected by a 1 km$^2$ detector like an expanded AMANDA., Comment: 9 pages, latex2e, 3 eps figures
Published: 1997
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30. Status of the AMANDA and BAIKAL neutrino telescopes

Author: Askebjer, P., Barwick, S. W., Bay, R., Bergström, L., Bouchta, A., Carius, Staffan, Dahlberg, E., Engel, K., Erlandsson, B., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Heukenkamp, H., Hulth, P. O., Hundertmark, S., Jacobsen, J., Johansson, S., Kandhadai, V., Karle, A., Liubarsky, I., Lowder, D., Mikolajski, T., Miller, T. C., Mock, P., Morse, R., Nygren, D., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Schneider, E., Spiering, C., Streicher, O., Sun, Q., Thon, T., Tilav, S., Walck, C., Wiebusch, C., Wischnewski, R., Yodh, G., Belolaptikov, I. A., Bezrukov, L. B., Borisovets, B. A., Budnev, N. M., Chensky, A. G., Danilchenko, I. A., Djilkibaev, Zh.-A.M., Dobrynin, V. I., Domogatsky, G. V., Doroshenko, A. A., Fialkovsky, S. V., Gaponenko, O. N., Garus, A. A., Gress, T. A., Ignat'ev, S. B., Klabukov, A. M., Klimov, A. I., Klimushin, S. I., Koshechkin, A. P., Kulepov, V. F., Kuzmichev, L. A., Lubsandorzhiev, B. K., Milenin, M. B., Mirgazov, R. R., Moroz, A. V., Moseiko, N. I., Nikiforov, S. A., Osipova, E. A., Pandel, D., Panfilov, A. I., Parfenov, Yu.V., Pavlov, A. A., Petukhov, D. P., Pocheikin, K. A., Pokhil, P. G., Pokolev, P. A., Rosanov, M. I., Rubzov, V.Yu., Sinegovsky, S. I., Sokalski, I. A., Spiering, Ch., Tarashansky, B. A., Askebjer, P., Barwick, S. W., Bay, R., Bergström, L., Bouchta, A., Carius, Staffan, Dahlberg, E., Engel, K., Erlandsson, B., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Heukenkamp, H., Hulth, P. O., Hundertmark, S., Jacobsen, J., Johansson, S., Kandhadai, V., Karle, A., Liubarsky, I., Lowder, D., Mikolajski, T., Miller, T. C., Mock, P., Morse, R., Nygren, D., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Schneider, E., Spiering, C., Streicher, O., Sun, Q., Thon, T., Tilav, S., Walck, C., Wiebusch, C., Wischnewski, R., Yodh, G., Belolaptikov, I. A., Bezrukov, L. B., Borisovets, B. A., Budnev, N. M., Chensky, A. G., Danilchenko, I. A., Djilkibaev, Zh.-A.M., Dobrynin, V. I., Domogatsky, G. V., Doroshenko, A. A., Fialkovsky, S. V., Gaponenko, O. N., Garus, A. A., Gress, T. A., Ignat'ev, S. B., Klabukov, A. M., Klimov, A. I., Klimushin, S. I., Koshechkin, A. P., Kulepov, V. F., Kuzmichev, L. A., Lubsandorzhiev, B. K., Milenin, M. B., Mirgazov, R. R., Moroz, A. V., Moseiko, N. I., Nikiforov, S. A., Osipova, E. A., Pandel, D., Panfilov, A. I., Parfenov, Yu.V., Pavlov, A. A., Petukhov, D. P., Pocheikin, K. A., Pokhil, P. G., Pokolev, P. A., Rosanov, M. I., Rubzov, V.Yu., Sinegovsky, S. I., Sokalski, I. A., Spiering, Ch., and Tarashansky, B. A.
Published: 1997
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31. Optical properties of deep ice at the South Pole : Absorption

Author: Askebjer, P., Berwick, S. W., Bergström, L., Bouchta, A., Carius, Staffan, Dalberg, E., Engel, K., Erlandsson, B., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Heukenkamp, H., Hulth, P. O., Hundertmark, S., Jacobsen, J., Karle, A., Kandhadai, V., Liubarsky, I., Lowder, D., Miller, T., Mock, P., Morse, R. M., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Schneider, E., Spiering, C., Streicher, O., Sun, Q., Thon, T., Tilav, S., Wischnewski, R., Walck, C., Yodh, G. B., Askebjer, P., Berwick, S. W., Bergström, L., Bouchta, A., Carius, Staffan, Dalberg, E., Engel, K., Erlandsson, B., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Heukenkamp, H., Hulth, P. O., Hundertmark, S., Jacobsen, J., Karle, A., Kandhadai, V., Liubarsky, I., Lowder, D., Miller, T., Mock, P., Morse, R. M., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Schneider, E., Spiering, C., Streicher, O., Sun, Q., Thon, T., Tilav, S., Wischnewski, R., Walck, C., and Yodh, G. B.
Abstract: We discuss recent measurements of the wavelength-dependent absorption coefficients in deep South Pole ice. The method uses transit-time distributions of pulses from a variable-frequency laser sent between emitters and receivers embedded in the ice. At depths of 800-1000 m scattering is dominated by residual air bubbles, whereas absorption occurs both in ice itself and in insoluble impurities. The absorption coefficient increases approximately exponentially with wavelength in the measured interval 410-610 nm. At the shortest wavelength our value is approximately a factor 20 below previous values obtained for laboratory ice and lake ice; with increasing wavelength the discrepancy with previous measurements decreases. At ∼415 to ∼500 nm the experimental uncertainties are small enough for us to resolve an extrinsic contribution to absorption in ice: submicrometer dust particles contribute by an amount that increases with depth and corresponds well with the expected increase seen near the Last Glacial Maximum in Vostok and Dome C ice cores. The laser pulse method allows remote mapping of gross structure in dust concentration as a function of depth in glacial ice., Source: Scopus
Published: 1997

32. UV and optical light transmission properties in deep ice at the South Pole

Author: Askebjer, P., Barwick, S. W., Bergström, L., Bouchta, A., Carius, Staffan, Dalberg, E., Erlandsson, B., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Heukenkamp, H., Hulth, P. O., Hundertmark, S., Jacobsen, J., Kandhadai, V., Karle, A., Liubarsky, I., Lowder, D., Miller, T., Mock, P., Morse, R., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Schneider, E., Spiering, Ch., Streicher, O., Sun, Q., Thon, Th., Tilav, S., Wischnewski, R., Walck, C., Yodh, G., Askebjer, P., Barwick, S. W., Bergström, L., Bouchta, A., Carius, Staffan, Dalberg, E., Erlandsson, B., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Heukenkamp, H., Hulth, P. O., Hundertmark, S., Jacobsen, J., Kandhadai, V., Karle, A., Liubarsky, I., Lowder, D., Miller, T., Mock, P., Morse, R., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Schneider, E., Spiering, Ch., Streicher, O., Sun, Q., Thon, Th., Tilav, S., Wischnewski, R., Walck, C., and Yodh, G.
Abstract: Both absorption and scattering of light at wavelengths 410 to 610 nanometers were measured in the South Pole ice at depths 0.8 to 1 kilometer with the laser calibration system of the Antarctic Muon And Neutrino Detector Array (AMANDA). At the shortest wavelengths the absorption lengths exceeded 200 meters - an order of magnitude longer than has been reported for laboratory ice. The absorption shows a strong wavelength dependence while the scattering length is found to be independent of the wavelength, consistent with the hypothesis of a residual density of air bubbles in the ice. The observed linear decrease of the inverse scattering length with depth is compatible with an earlier measurement by the AMANDA collaboration (at ∼515 nanometers)., Art. No.: 97GL01246
Published: 1997

33. Revisiting Nucleosynthesis Constraints on Primordial Magnetic Fields

Author: Grasso, D., Rubinstein, H. R., Grasso, D., and Rubinstein, H. R.
Abstract: In view of several conflicting results, we reanalyze the effects of magnetic fields on the primordial nucleosynthesis. In the case the magnetic field is homogeneous over a horizon volume, we show that the main effects of the magnetic field are given by the contribution of its energy density to the Universe expansion rate and the effect of the field on the electrons quantum statistics. Although, in order to get an upper limit on the field strength, the weight of the former effect is numerically larger, the latter cannot be neglected. Including both effects in the PN code we get the upper limit $B \le 1\times 10^{11}$ Gauss at the temperature $T = 10^9~^oK$. We generalize the considerations to cases when instead the magnetic is inhomogeneous on the horizon length. We show that in these cases only the effect of the magnetic field on the electrons statistics is relevant. If the coherence length of the magnetic field at the end of the PN is in the range $10 \ll L_0 \ll 10^{11}$ cm our upper limit is $B \le 1\times 10^{12}$ Gauss., Comment: 12 pages LaTex file with two included ps figs
Published: 1996
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34. Revisiting Nucleosynthesis Constraints on Primordial Magnetic Fields

Author: Grasso, D., Rubinstein, H. R., Grasso, D., and Rubinstein, H. R.
Abstract: In view of several conflicting results, we reanalyze the effects of magnetic fields on the primordial nucleosynthesis. In the case the magnetic field is homogeneous over a horizon volume, we show that the main effects of the magnetic field are given by the contribution of its energy density to the Universe expansion rate and the effect of the field on the electrons quantum statistics. Although, in order to get an upper limit on the field strength, the weight of the former effect is numerically larger, the latter cannot be neglected. Including both effects in the PN code we get the upper limit $B \le 1\times 10^{11}$ Gauss at the temperature $T = 10^9~^oK$. We generalize the considerations to cases when instead the magnetic is inhomogeneous on the horizon length. We show that in these cases only the effect of the magnetic field on the electrons statistics is relevant. If the coherence length of the magnetic field at the end of the PN is in the range $10 \ll L_0 \ll 10^{11}$ cm our upper limit is $B \le 1\times 10^{12}$ Gauss., Comment: 12 pages LaTex file with two included ps figs
Published: 1996
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35. Revisiting Nucleosynthesis Constraints on Primordial Magnetic Fields

Author: Grasso, D., Rubinstein, H. R., Grasso, D., and Rubinstein, H. R.
Abstract: In view of several conflicting results, we reanalyze the effects of magnetic fields on the primordial nucleosynthesis. In the case the magnetic field is homogeneous over a horizon volume, we show that the main effects of the magnetic field are given by the contribution of its energy density to the Universe expansion rate and the effect of the field on the electrons quantum statistics. Although, in order to get an upper limit on the field strength, the weight of the former effect is numerically larger, the latter cannot be neglected. Including both effects in the PN code we get the upper limit $B \le 1\times 10^{11}$ Gauss at the temperature $T = 10^9~^oK$. We generalize the considerations to cases when instead the magnetic is inhomogeneous on the horizon length. We show that in these cases only the effect of the magnetic field on the electrons statistics is relevant. If the coherence length of the magnetic field at the end of the PN is in the range $10 \ll L_0 \ll 10^{11}$ cm our upper limit is $B \le 1\times 10^{12}$ Gauss., Comment: 12 pages LaTex file with two included ps figs
Published: 1996
Full Text: View/download PDF

36. Revisiting Nucleosynthesis Constraints on Primordial Magnetic Fields

Author: Grasso, D., Rubinstein, H. R., Grasso, D., and Rubinstein, H. R.
Abstract: In view of several conflicting results, we reanalyze the effects of magnetic fields on the primordial nucleosynthesis. In the case the magnetic field is homogeneous over a horizon volume, we show that the main effects of the magnetic field are given by the contribution of its energy density to the Universe expansion rate and the effect of the field on the electrons quantum statistics. Although, in order to get an upper limit on the field strength, the weight of the former effect is numerically larger, the latter cannot be neglected. Including both effects in the PN code we get the upper limit $B \le 1\times 10^{11}$ Gauss at the temperature $T = 10^9~^oK$. We generalize the considerations to cases when instead the magnetic is inhomogeneous on the horizon length. We show that in these cases only the effect of the magnetic field on the electrons statistics is relevant. If the coherence length of the magnetic field at the end of the PN is in the range $10 \ll L_0 \ll 10^{11}$ cm our upper limit is $B \le 1\times 10^{12}$ Gauss., Comment: 12 pages LaTex file with two included ps figs
Published: 1996
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37. Particle astrophysics in antarctica

Author: Miller, T. C., Evenson, Paul A., Gaisser, T. K., Martello, D., Spiczak, G. M., Stanev, T., Dickinson, E., Gill, J. R., Hart, S., Hinton, J., Lloyd-Evans, J., Ogden, P. A., Patel, M., Pryke, C. L., Watson, A. A., Lowder, D. M., Price, P. B., Richards, A., Nygren, D., Barwick, S. W., Mock, P., Porrata, R., Schneider, E., Askebjer, P., Bergstrom, L., Bouchta, A., Dahlberg, E., Ekstrom, P., Erlandsson, B., Goobar, A., Hulth, P. O., Sun, Q, Walck, C., Carius, Staffan, Hallgren, A., Rubinstein, H., Engel, K., Gray, L., Halzen, F., Jacobsen, J., Kandhadai, V., Liubarsky, I., Morse, R., Tilav, S., Heukenkamp, S., Hundertmark, S., Karle, A., Thon, T., Spiering, C., Streicher, O., Wiebusch, C., Wischenewski, R., Miller, T. C., Evenson, Paul A., Gaisser, T. K., Martello, D., Spiczak, G. M., Stanev, T., Dickinson, E., Gill, J. R., Hart, S., Hinton, J., Lloyd-Evans, J., Ogden, P. A., Patel, M., Pryke, C. L., Watson, A. A., Lowder, D. M., Price, P. B., Richards, A., Nygren, D., Barwick, S. W., Mock, P., Porrata, R., Schneider, E., Askebjer, P., Bergstrom, L., Bouchta, A., Dahlberg, E., Ekstrom, P., Erlandsson, B., Goobar, A., Hulth, P. O., Sun, Q, Walck, C., Carius, Staffan, Hallgren, A., Rubinstein, H., Engel, K., Gray, L., Halzen, F., Jacobsen, J., Kandhadai, V., Liubarsky, I., Morse, R., Tilav, S., Heukenkamp, S., Hundertmark, S., Karle, A., Thon, T., Spiering, C., Streicher, O., Wiebusch, C., and Wischenewski, R.
Published: 1996

38. Dependence of Lattice Hadron Masses on External Magnetic Fields

Author: Rubinstein, H. R., Solomon, S., Wittlich, T., Rubinstein, H. R., Solomon, S., and Wittlich, T.
Abstract: We study the variation of the hadron masses in the presence of external magnetic fields of strength of the order of the masses themselves. We identify the main factors affecting the lattice simulation results: - the boundary discontinuities for $eB << 2\pi / L^2 a^2$. - the SU(6) choice of the hadron wave-function. We confirm qualitatively the earlier theoretical ansatz on the linear behaviour of the masses with the magnetic field and, as a by-product, we improve the lattice measurements of the nucleon magnetic moments. However our systematic and statistical errors preclude us from measuring the theoretically predicted field strength at which the proton becomes heavier than the neutron., Comment: 18 pages, compressed uuencoded postscript file
Published: 1995
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39. Dependence of Lattice Hadron Masses on External Magnetic Fields

Author: Rubinstein, H. R., Solomon, S., Wittlich, T., Rubinstein, H. R., Solomon, S., and Wittlich, T.
Abstract: We study the variation of the hadron masses in the presence of external magnetic fields of strength of the order of the masses themselves. We identify the main factors affecting the lattice simulation results: - the boundary discontinuities for $eB << 2\pi / L^2 a^2$. - the SU(6) choice of the hadron wave-function. We confirm qualitatively the earlier theoretical ansatz on the linear behaviour of the masses with the magnetic field and, as a by-product, we improve the lattice measurements of the nucleon magnetic moments. However our systematic and statistical errors preclude us from measuring the theoretically predicted field strength at which the proton becomes heavier than the neutron., Comment: 18 pages, compressed uuencoded postscript file
Published: 1995
Full Text: View/download PDF

40. Dependence of Lattice Hadron Masses on External Magnetic Fields

Author: Rubinstein, H. R., Solomon, S., Wittlich, T., Rubinstein, H. R., Solomon, S., and Wittlich, T.
Abstract: We study the variation of the hadron masses in the presence of external magnetic fields of strength of the order of the masses themselves. We identify the main factors affecting the lattice simulation results: - the boundary discontinuities for $eB << 2\pi / L^2 a^2$. - the SU(6) choice of the hadron wave-function. We confirm qualitatively the earlier theoretical ansatz on the linear behaviour of the masses with the magnetic field and, as a by-product, we improve the lattice measurements of the nucleon magnetic moments. However our systematic and statistical errors preclude us from measuring the theoretically predicted field strength at which the proton becomes heavier than the neutron., Comment: 18 pages, compressed uuencoded postscript file
Published: 1995
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41. On the age vs depth and optical clarity of deep ice at South Pole

Author: Askebjer, P., Barwick, S., Bergstrom, L., Bouchta, A., Carius, Staffan, Coulthard, A., Engel, K., Erlandsson, B., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Hulth, P. O., Jacobsen, J., Johansson, S., Kandhadai, V., Liubarsky, I., Lowder, D., Miller, T., Mock, P. C., Morse, R., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Spang, J. C., Sun, Q., Tilav, S., Walck, C., Yodh, G., Askebjer, P., Barwick, S., Bergstrom, L., Bouchta, A., Carius, Staffan, Coulthard, A., Engel, K., Erlandsson, B., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Hulth, P. O., Jacobsen, J., Johansson, S., Kandhadai, V., Liubarsky, I., Lowder, D., Miller, T., Mock, P. C., Morse, R., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Spang, J. C., Sun, Q., Tilav, S., Walck, C., and Yodh, G.
Abstract: The first four strings of phototubes for the AMANDA high-energy neutrino observatory are now frozen in place at a depth of 800 to 1000 m in ice at the South Pole. During the 1995-96 season an additional six strings will be deployed at greater depths. Provided absorption, scattering, and refraction of visible light are sufficiently small, the trajectory of a muon into which a neutrino converts can be determined by using the array of phototubes to measure the arrival times of \v{C}erenkov light emitted by the muon. To help in deciding on the depth for implantation of the six new strings, we discuss models of age vs depth for South Pole ice, we estimate mean free paths for scattering from bubbles and dust as a function of depth, and we assess distortion of light paths due to refraction at crystal boundaries and interfaces between air-hydrate inclusions and normal ice. We conclude that the depth interval 1600 to 1800 m will be suitably transparent for the next six AMANDA strings and, moreover, that the interval 1600 to 2100 m will be suitably transparent for a future 1-km 3 observatory except possibly in a region a few tens of meters thick at a depth corresponding to a peak in the dust concentration at 60 kyr BP.
Published: 1995

42. Initial analysis of coincident events between the SPASE and AMANDA detectors

Author: Miller, T., Beaman, J., Evenson, P. A., Gaisser, T. K., Hart, S., Lloyd-Evans, J., Martello, D., Ogden, P., Petrakis, J., Stanev, T., Watson, A. A., Askebjer, P., Barwick, S. W., Bergström, L., Bouchta, A., Carius, Staffan, Erlandsson, B., Goobar, A., Gray, L., Hallgren, L. A., Halzen, F., Hulth, P. O., Jacobsen, J., Johansson, S., Kandhadai, V., Liubarsky, I., Lowder, D. M., Mock, P., Morse, R., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Sun, Q., Tilav, S., Walck, C., Yodh, G., Miller, T., Beaman, J., Evenson, P. A., Gaisser, T. K., Hart, S., Lloyd-Evans, J., Martello, D., Ogden, P., Petrakis, J., Stanev, T., Watson, A. A., Askebjer, P., Barwick, S. W., Bergström, L., Bouchta, A., Carius, Staffan, Erlandsson, B., Goobar, A., Gray, L., Hallgren, L. A., Halzen, F., Hulth, P. O., Jacobsen, J., Johansson, S., Kandhadai, V., Liubarsky, I., Lowder, D. M., Mock, P., Morse, R., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Sun, Q., Tilav, S., Walck, C., and Yodh, G.
Abstract: We report on the status of the SPASE-AMANDA coincidence experiment., Source: Scopus
Published: 1995
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43. AMANDA : status report from the 1993-94 campaign and optical properties of the South Pole ice

Author: Askebjer, P., Barwick, S. W., Bergström, L., Bouchta, A., Carius, Staffan, Coulthard, A., Engel, K., Erlandsson, B., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Hulth, P. O., Jacobsen, J., Johansson, S., Kandhadai, V., Liubarsky, I., Lowder, D., Miller, T., Mock, P., Morse, R., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Schneider, E., Sun, Q., Tilav, S., Walck, C., Yodh, G., Askebjer, P., Barwick, S. W., Bergström, L., Bouchta, A., Carius, Staffan, Coulthard, A., Engel, K., Erlandsson, B., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Hulth, P. O., Jacobsen, J., Johansson, S., Kandhadai, V., Liubarsky, I., Lowder, D., Miller, T., Mock, P., Morse, R., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Schneider, E., Sun, Q., Tilav, S., Walck, C., and Yodh, G.
Abstract: We report the first results of the AMANDA detector. During the antarctic summer 1993-94 four strings were deployed between 0.8 an 1 km depth, each equipped with 20 photomultiplier tubes (PMTs). A laser source was used to investigate the optical properties of the ice in situ. We find that the ice is intrinsically extremely transparent. The measured absorption length is 59 ± 3 m, i.e. comparable with the quality of the ultra-pure water used in the IMB and Kamiokande proton-decay and neutrino experiments [1,2] and more than two times longer than the best value reported for laboratory ice [3]. Due to a residual density of air bubbles at these depths, the motion of photons in the medium is randomized. For spherical, smooth bubbles we find that, at 1 km depth, the average distance between collisions is about 25 cm. The measured inverse scattering length on bubbles decreases linearly with increasing depth in the volume of ice investigated. © 1995 Elsevier Science B.V. All rights reserved., Source: Scopus
Published: 1995
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44. Optical properties of the South Pole ice at depths between 0.8 and 1 kilometer

Author: Askebjer, P., Barwick, S. W., Bergström, L., Bouchta, A., Carius, Staffan, Coulthard, A., Engel, K., Erlandsson, B., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Hulth, P. O., Jacobsen, J., Johansson, S., Kandhadai, V., Liubarsky, I., Lowder, D., Miller, T., Mock, P. C., Morse, R., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Schneider, E., Sun, Q., Tilav, S., Walck, C., Yodh, G., Askebjer, P., Barwick, S. W., Bergström, L., Bouchta, A., Carius, Staffan, Coulthard, A., Engel, K., Erlandsson, B., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Hulth, P. O., Jacobsen, J., Johansson, S., Kandhadai, V., Liubarsky, I., Lowder, D., Miller, T., Mock, P. C., Morse, R., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Schneider, E., Sun, Q., Tilav, S., Walck, C., and Yodh, G.
Abstract: The optical properties of the ice at the geographical South Pole have been investigated at depths between 0.8 and 1 kilometer. The absorption and scattering lengths of visible light (∼515 nanometers) have been measured in situ with the use of the laser calibration setup of the Antarctic Muon and Neutrino Detector Array (AMANDA) neutrino detector. The ice is intrinsically extremely transparent. The measured absorption length is 59 ± 3 meters, comparable with the quality of the ultrapure water used in the Irvine-Michigan-Brookhaven and Kamiokande proton-decay and neutrino experiments and more than twice as long as the best value reported for laboratory ice. Because of a residual density of air bubbles at these depths, the trajectories of photons in the medium are randomized. If the bubbles are assumed to be smooth and spherical, the average distance between collisions at a depth of 1 kilometer is about 25 centimeters. The measured inverse scattering length on bubbles decreases linearly with increasing depth in the volume of ice investigated., Source: Scopus
Published: 1995

45. Status and capabilities of AMANDA-94

Author: Mock, P. C., Askebjer, P., Barwick, S.W., Bergstrom, L., Bouchta, A., Carius, Staffan, Erlandsson, A., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Heukenkamp, H., Hulth, P. O., Jacobsen, J., Johansson, S., Kandhadai, V., Karle, A., Liubarsky, I., Lowder, D. M., Miller, T. C., Morse, R., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Spiering, C., Sun, Q., Thon, T., Tilav, S., Walck, C., Wischnewiski, R., Yodh, G., Mock, P. C., Askebjer, P., Barwick, S.W., Bergstrom, L., Bouchta, A., Carius, Staffan, Erlandsson, A., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Heukenkamp, H., Hulth, P. O., Jacobsen, J., Johansson, S., Kandhadai, V., Karle, A., Liubarsky, I., Lowder, D. M., Miller, T. C., Morse, R., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Spiering, C., Sun, Q., Thon, T., Tilav, S., Walck, C., Wischnewiski, R., and Yodh, G.
Published: 1995

46. A System to search for supernova bursts with the AMANDA detector

Author: Wischnewski, R., Askebjer, P., Barwick, S. W., Bergstrom, L., Bouchta, A., Carius, Staffan, Erlandsson, B., Goodbar, A., Gray, L., Hallgren, A., Halzen, F., Heukenkamp, H., Hulth, P. O., Jacobsen, J., Johansson, S., Kandhadai, V., Karle, A., Liubarsky, I., Lowder, D. M., Miller, T. C., Mock, P. C., Morse, R., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Spiering, C., Sun, Q., Thon, T., Tilav, S., Walack, C., Yodh, G., Wischnewski, R., Askebjer, P., Barwick, S. W., Bergstrom, L., Bouchta, A., Carius, Staffan, Erlandsson, B., Goodbar, A., Gray, L., Hallgren, A., Halzen, F., Heukenkamp, H., Hulth, P. O., Jacobsen, J., Johansson, S., Kandhadai, V., Karle, A., Liubarsky, I., Lowder, D. M., Miller, T. C., Mock, P. C., Morse, R., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Spiering, C., Sun, Q., Thon, T., Tilav, S., Walack, C., and Yodh, G.
Published: 1995

47. Indirect evidence for long absorption lengths in Antarctic ice

Author: Tilav, S., Askebjer, P., Barwick, S. W., Bergstrom, L., Bouchta, A., Carius, Staffan, Erlandsson, B., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Heukenkamp, H., Hulth, P. O., Jacobsen, J., Johansson, S., Kandhadai, V., Karle, A., Liubarsky, I., Lowder, D. M., Martello, D., Miller, T. C., Mock, P. C., Morse, R., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Spiering, C., Sun, Q., Thon, T., Walck, C., Wischnewski, R., Yodh, G., Tilav, S., Askebjer, P., Barwick, S. W., Bergstrom, L., Bouchta, A., Carius, Staffan, Erlandsson, B., Goobar, A., Gray, L., Hallgren, A., Halzen, F., Heukenkamp, H., Hulth, P. O., Jacobsen, J., Johansson, S., Kandhadai, V., Karle, A., Liubarsky, I., Lowder, D. M., Martello, D., Miller, T. C., Mock, P. C., Morse, R., Porrata, R., Price, P. B., Richards, A., Rubinstein, H., Spiering, C., Sun, Q., Thon, T., Walck, C., Wischnewski, R., and Yodh, G.
Published: 1995

48. Neutrino Fluxes and Resonance Physics with Neutrino Telescopes

Author: Bander, Myron, Rubinstein, H. R., Bander, Myron, and Rubinstein, H. R.
Abstract: Expected atmospheric ${\bar \nu_e}$ fluxes will result in a significant number of resonantly produced low mass hadronic vector states, as the $\rho$, in large volume neutrino telescopes. The existence of sources of higher energy neutrinos will result in the production of higher mass states, as the $D_s^*$ and the $({\bar t}b)_{J=1}$. We calculate the rates of production of these states and discuss their signals. Independent of theoretical flux determinations, the detection of these states will be a tool for experimentally determining these fluxes., Comment: pages, UCI-TR 94-10
Published: 1994
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49. Nucleon masses in strong magnetic fields

Author: Rubinstein, H. R., Solomon, S., Wittlich, T., Rubinstein, H. R., Solomon, S., and Wittlich, T.
Abstract: We compute the variation of the masses of the proton and the neutron induced by the presence of a strong external magnetic field. We discuss the choice of the wave function and different techniques how to apply the magnetic field. The results obtained from a 24 16^2 8 and a 16^2 8^2 lattice are compared with a phenomenological approach., Comment: 3 pages, PostScipt, compressed, uuencoded, contribution to Lattice 94
Published: 1994
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50. Nucleon masses in strong magnetic fields

Author: Rubinstein, H. R., Solomon, S., Wittlich, T., Rubinstein, H. R., Solomon, S., and Wittlich, T.
Abstract: We compute the variation of the masses of the proton and the neutron induced by the presence of a strong external magnetic field. We discuss the choice of the wave function and different techniques how to apply the magnetic field. The results obtained from a 24 16^2 8 and a 16^2 8^2 lattice are compared with a phenomenological approach., Comment: 3 pages, PostScipt, compressed, uuencoded, contribution to Lattice 94
Published: 1994
Full Text: View/download PDF

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