The R.A.P.Project "Prosto o slozhnom" "Astro-ph za vtoruyu polovinu 2003 g." Nemnogo statistiki Predydushii vypusk (N117) Slovar' astroterminov Spisok missii i teleskopov Obzory UFN Stat'i SOZh ANKa Dnya 06.05.2005. Dalekoe kol'co Einshteina 07.04.2005. Disk vokrug Vegi 26.03.2005. Ten' Luny 23.03.2005. Novyi rentgenovskii pul'sar v ostatke sverhnovoi 22.03.2005. Eshe o blinnoi teorii ... Soderzhanie i bystryi perehod k razdelam obzora Stat'i nedeli "Luchshie iz luchshih" astro-ph/0510412 Zvezdy, obrazovannye v rezul'tate gravitacionnogo kollapsa, a ne akkrecii physics/0510188 Matematika, materiya i myshlenie astro-ph/0510687 Novyi mehanizm vzryvov sverhnovyh Otdel'nye stat'i Akkreciya Bondi-Hoila iz turbulentnoi sredy Novoe rassmotrenie i ocenka neopredelennostei v modelyah populyacionnogo sinteza Zvezdy, obrazovannye v rezul'tate gravitacionnogo kollapsa, a ne akkrecii Nablyudeniya solnechnopodobnyh oscillyacii: svezhie rezul'taty Velikolepnaya semerka: blizkie odinochnye neitronnye zvezdy s sil'nymi magnitnymi polyami Registraciya goryachego kompan'ona eta Karina Obzor pul'sarov v oblastyah lokalizacii istochnikov EGRET Prichiny i sledstviya izmeneniya magnitnyh polei neitronnyh zvezd Kosmicheskie luchi sverhvysokih energii i observatoriya Ozhe Kollaps zamagnichennyh gipermassivnyh neitronnyh zvezd s uchetov effektov OTO Shlopyvayutsya li neitronnye zvezdy? Anizotropnoe teplovoe izluchenie zamagnichennyh neitronnyh zvezd Novyi mehanizm vzryvov sverhnovyh Postroenie teplovoi i magnitnoi karty poverhnosti neitronnoi zvezdy po ee rentgenovskomu izlucheniyu: metod i analiz krivyh bleska Iz razdela physics Global'noe povedenie indeksa produktivnosti issledovatelei Matematika, materiya i myshlenie Polnyi Arhiv predydushih vypuskov. Arhiv statei, voshedshih v vypuski s 01 iyulya 2002 g. po 31 marta 2003 g. Razdely arhiva (s aprelya 2003 g.): kosmologiya, neitrino, kosmicheskie luchi i gamma-astronomiya, galaktiki, AYaG, kvazary, nasha Galaktika, mezhzvezdnaya sreda, zvezdy, sverhnovye, ostatki sverhnovyh, chernye dyry, neitronnye zvezdy, linzirovanie, Solnce, ekzoplanety, Solnechnaya sistema, akkreciya, tesnye dvoinye sistemy, gamma-vspleski, gravitacionnye volny, mehanizmy izlucheniya, chislennoe modelirovanie, dinamika, mehanika metody obrabotki dannyh, MGD, metody nablyudenii, budushie nablyudatel'nye proekty, prochee. Poleznye astronomicheskie ssylki. Korotkoe esse ob elektronnyh preprintah. Obzornye stat'i v astro-ph 2001-2003 gg. Obsudit' na forume Scientific.RU Obsudit' na forume Zvezdocheta Avtor proekta Sergei Popov Diskussii po stat'yam Arhiva PhysComments CosmoCoffee Postav'te u sebya nashu knopku! Proekt razmeshen na saitah: Vy mozhet takzhe razmestit' na svoem saite nashu lentu obzorov Novostnye lenty Novosti astronomii ot PRAO Novosti kosmonavtiki Novosti ot UFN Astronomer.Ru Informnauka Researcher@ Elementy.Ru Grani.Ru Perst Podpiska na rassylku obzorov na Subscribe.Ru Druzhestvennye rassylki: "Astronomiya segodnya" "Astronomiya dlya shkol'nikov" "Okno vo Vselennuyu" Spisok astrorassylok

Obzory preprintov astro-ph Vypusk N118 astro-ph za 17 - 28 oktyabrya 2005 goda: izbrannye stat'i Referaty otdel'nyh statei astro-ph/0510410 Akkreciya Bondi-Hoila iz turbulentnoi sredy (Bondi-Hoyle Accretion in a Turbulent Medium) Authors: Mark R. Krumholz et al. Comments: Accepted for publication in ApJ; 13 pages, 9 figures, emulateapj Klassicheskaya formula akkrecii Bondi neprimenima v sluchae sil'no turbulizovannoi sredy. Avtory obsuzhdayut, kak sil'naya sverhzvukovaya turbulentnost' povliyaet na temp akkrecii. Effekty turbulentnosti dostatochno slozhno uchest'. Dazhe vyvody raboty trudno chetko i kratko sformulirovat'. Vozmozhna situaciya, kogda temp budet vyshe, chem formal'no vychislennyi po formule Bondi, vozmozhna i obratnaya situaciya. Otmechu, chto avtory prenebregali rol'yu magnitnyh polei. Uchest' srazu i turbulentnost' i polya budet ochen' slozhno dazhe v chislennyh raschetah. Avtory prilagayut svoi raschety k formirovaniyu molodyh zvezd (sm. bolee podrobno stat'yu teh zhe avtorov nizhe - astro-ph/0510412) i akkrecii na zvezdy do stadii glavnoi posledovatel'nosti. Pokazano, chto dlya massivnyh ob'ektov vozmozhno sushestvennoe izmenenie po-sravneniyu s bolee rannimi modelyami. Krome togo, kratko rassmotrena akkreciya na sverhmassivnye chernye dyry v centrah galaktik. obzor astro-ph/0510411 Novoe rassmotrenie i ocenka neopredelennostei v modelyah populyacionnogo sinteza (Revisiting and assessing uncertainties in stellar populations synthesis models) Authors: M. Cervino, V. Luridiana Comments: 35 pages, 16 figures. Invited review to "Resolved Stellar Populations", Cancun (Mexico) Apr 2005. To appear on the proceedings of the conference edited by D. Valls-Gabaud & M. Chavez, ASP Conf. Ser. (ASP: San Francisco) Podrobno obsuzhdaetsya odin iz vazhnyh aspektov populyacionnyh modelei v astrofizike. astro-ph/0510412 Zvezdy, obrazovannye v rezul'tate gravitacionnogo kollapsa, a ne akkrecii (Stars Form By Gravitational Collapse, Not Competitive Accretion) Authors: Mark R. Krumholz et al. Comments: Accepted for publication in Nature; 13 pages, no figures, Nature manuscript style Avtory obsuzhdayut dve populyarnye na segodnyashnii den' modeli obrazovaniya zvezd. V pervoi vse proishodit tak. Molekulyarnye oblaka raspadayutsya na gazovye sgustki (yadra), kotorye zatem kollapsiruyut. Sootvetstvenno, massa sgustka opredelyaet massu zvezdy. Vo vtoroi iznachal'no obrazuyutsya yadra primerno odinakovogo razmera, a zatem ih massa uvelichivaetsya putem akkrecii. Sootvetstvenno burye (korichnevye) karliki ob'yasnyayutsya v takoi modeli vybrosom yadra do togo, kak ego massa sushestvenno vozrosla. V stat'e pokazano (a stat'ya-to, zamet'te, prinyata k publikacii v Nature!), chto v real'nyh oblastyah zvezdoobrazovaniya akkreciya budet nedostatochno sil'na. T.o., utverzhdayut avtory, imenno model' kollapsa "edinstvenno vernaya". miniobzor astro-ph/0510416 Nablyudeniya solnechnopodobnyh oscillyacii: svezhie rezul'taty (Observing solar-like oscillations: recent results) Authors: Timothy R. Bedding, Hans Kjeldsen Comments: 6 pages, Invited review talk at the meeting on Stellar Pulsation and Evolution, June 2005, Rome. Proceedings to appear in "Memorie della Societa' Astronomica Italiana", Vol. 76/4, eds. A.R. Walker & G. Bono Vot uzhe neskol'ko let kak astroseismologi aktivno i uspeshno izuchayut ne tol'ko Solnce, no i blizkie zvezdy. V stat'e predstavlen kratkii obzor poslednih dostizhenii, problem i planov astroseismologov. miniobzor astro-ph/0510480 Velikolepnaya semerka: blizkie odinochnye neitronnye zvezdy s sil'nymi magnitnymi polyami (The Magnificent Seven: Nearby Isolated Neutron Stars with strong Magnetic Fields) Authors: F. Haberl Comments: Proceedings of the 2005 EPIC XMM-Newton Consortium Meeting, Ringberg Castle, Germany, April 11-13 2005, Edt. U.G. Briel, S. Sembay and A. Read, MPE Report 288, June 2005 Dana svodka sovremennyh nablyudatel'nyh dannyh po Velikolepnoi semerke. Priyatno, chto predlozhennoe nami imya vse-taki prizhilos' :) Po vsei vidimosti, eto ob'ekty s dostatochno sil'nym magnitnym polem 1013-1014 Gs. astro-ph/0510581 Registraciya goryachego kompan'ona eta Karina (Detection of a Hot Binary Companion of $\eta$ Carinae) Authors: Rosina C. Iping et al. Comments: 13 pages with figures To, chto izvestnaya zvezda eta Kilya (Carina) yavlyaetsya dvoinoi v principe izvestno dostatochno davno. Odnako do sih por ne udavalos' pryamo vydelit' izluchenie bolee slabogo komponenta. S pomosh'yu sputnika FUSE (Far Ultraviolet Spectroscopic Explorer) udalos' vo vremya rentgenovskogo zatmeniya vydelit' spektr goryachego komponenta. Nesmotrya na to, chto komponent A dominiruet v optike, v dalekom ul'trafiolete pochti vse izluchenie svyazano s bolee goryachim kompan'onom V. Po parametram spektral'nyh linii udalos' postavit' nekotorye ogranichenie na parametry vtoroi zvezdy sistemy. V chastnosti, skorost' zvezdnogo vetra okazalas' v neskol'ko raz nizhe predskazyvavsheisya. astro-ph/0510608 Obzor pul'sarov v oblastyah lokalizacii istochnikov EGRET (A survey for pulsars in EGRET error boxes) Authors: D. J. Champion, M. A. McLaughlin, D. R. Lorimer Comments: 5 pages, 1 figure. Accepted for publication in MNRAS Na bol'shom radioteleskope v Aresibo proveden poisk pul'sarov v 19 oblastyah lokalizacii istochnikov, obnaruzhennyh priborom EGRET na bortu CGRO. Predpolagaetsya, chto eti istochniki mogut byt' svyazany s Poyasom Gulda. V hode poiska obnaruzhen odin novyi pul'sar, odnako avtory polagayut, chto on ne svyazan s gamma-istochnikom. T.o., osnovyvayas' na negativnyh rezul'tatah poiska, avtory zaklyuchayut, chto ili neotozhdestvlennye istochniki EGRET, svyazannye s Poyasom gulda ne yavlyayutsya radiopul'sarami, ili zhe ih svetimost' anomal'no mala. obzor astro-ph/0510623 Prichiny i sledstviya izmeneniya magnitnyh polei neitronnyh zvezd (Causes and Consequences of Magnetic Field Changes in Neutron Stars) Authors: M. Ruderman Comments: 17 pages, 19 figures Ruderman - klassik fiziki neitronnyh zvezd. V etoi stat'e on rassmatrivaet vozmozhnye scenarii evolyucii magnitnogo polya neitronnyh zvezd. V osnove rassmotreniya lezhit ideya o tom, chto v ne ochen' molodoi neitronnoi zvezde (starshe primerno tysyachi let) proishodit sleduyushee. Sverhtekuchie neitrony, chtoby uchastvovat' vo vrashenii zvezdy, obyazany obrazovat' vihrevye niti. V processe zamedleniya (uskoreniya) eti niti budut dvigat' ot centra zvezdy naruzhu (vnutr'). Magnitnoe pole, v svoyu ochered', takzhe porozhdaet pohozhie struktury, no uzhe iz protonov. Formiruyutsya kvantovye "trubki", v kotoryh i sosredotocheno pole. Magnitnye trubki mogut vzaimodeistvovat' s vihrevymi nityami. V processe svoego smesheniya vihrevye niti tyanut trubki za soboi. Sootvetstvenno, izmenyaetsya topologiya magnitnogo polya. Rassmotreno, kak takaya evolyuciya mozhet vyglyadet' na diagramme period - proizvodnaya perioda. Takzhe obsuzhdaetsya svyaz' glitchei s vzaimodeistviem nitei i trubok. miniobzor astro-ph/0510627 Kosmicheskie luchi sverhvysokih energii i observatoriya Ozhe (Ultra High Energy Cosmic Rays and the Auger Observatory) Authors: Antoine Letessier-Selvon Comments: 12 pages, 7 figures. Proceedings of the PIC 2005 conference. Praha, July 2005 Ocherednoi obzor, posvyashennyi observatorii imeni P'era Ozhe. Krome opisaniya dizaina i celei predstavleny pervye rezul'taty. Dlya teh, kto eshe ne uspel poznakomit'sya so vsem etim, budet ochen' interesno, t.k. imenno eta observatoriya v blizhaishie neskol'ko let prizvana reshit' zagadku kosmicheskih luchei sverhvysokih energii. astro-ph/0510653 Kollaps zamagnichennyh gipermassivnyh neitronnyh zvezd s uchetov effektov OTO (Collapse of magnetized hypermassive neutron stars in general relativity) Authors: Matthew D. Duez et al. Comments: Submitted to Phys. Rev. Lett Vot uzhe bolee 20 let aktivno obsuzhdayutsya vozmozhnye nablyudatel'nye proyavleniya sliyanii neitronnyh zvezd. Problema sostoit v ochen' slozhnyh processah, proishodyashih pri etom. Tak, neizvestno, chto zhe obrazuetsya v rezul'tate sliyaniya. Odnoi iz vozmozhnostei yavlyaetsya formirovanie t.n. gipermassivnyh neitronnyh zved, kotorye vposledstvii kollapsiruyut v chernye dyry. Pristavka "giper" otrazhaet tot fakt, chto obrazovavshiisya kompaktnyi ob'ekt imeet netipichno bol'shuyu massu. V samom dele, standartnye modeli govoryat, chto udvoenie massy neitronnoi zvezdy privedet k ee kollapsu (tipichnaya massa pul'sara poryadka 1.3-1.5 mass solnca, a massy bolee 2 solnechnyh uzhe mogut privodit' k kollapsu). Odnako eto prilozhimo k obychnym - holodnym i dovol'no medlenno vrashayushimsya - neitronnym zvezdam. Posle sliyaniya zhe obrazuetsya ochen' bystro vrashayushiisya (prichem differencial'no vrashayushiisya!) goryachii ob'ekt. Eti svoistva yavlyayutsya dopolnitel'nymi istochnikami ustoichivosti (v stat'e rassmotrena situaciya, v kotoroi imenno differencial'noe vrashenie stabiliziruet kompaktnyi ob'ekt). Na kakoe-to vremya neitronnaya zvezda mozhet izbezhat' kollapsa, kotoryi, odnako, neizbezhen. Avtory proveli detal'noe modelirovanie s uchetom magnitnyh polei i effektov obshei teorii otnositel'nosti. Raschety pokazyvayut, chto kollaps gipermassivnoi neitronnoi zvezdy v chernuyu dyru mozhet yavlyat'sya horoshim kandidatom v mehanizmy, otvechayushie za korotkie gamma-vspleski. O drugom mehanizme takih vspleskov, svyazannom s obrazovaniem kvarkovoi zvezdy, sm. v stat'e astro-ph/0510691, o kotoroi my ne budem detal'no rasskazyvat' v obzore. Krome togo, sliyaniyam neitronnyh zvezd posvyasheno eshe neskol'ko svezhih statei. V rabote astro-ph/0510682 rech' idet ob ostatkah sliyanii, no ne v smysle "kompaktnyi ostatok", a ob analogah ostatkov vzryvov sverhnovyh - vybroshennyh obolochkah. Pro etu rabotu ya takzhe ne budu detal'no rasskazyvat', a obrashu vnimanie chitatelya na sleduyushuyu stat'yu - astro-ph/0510668. astro-ph/0510668 Shlopyvayutsya li neitronnye zvezdy? (Are neutron stars crushed? Gravitomagnetic tidal fields as a mechanism for binary-induced collapse) Authors: Marc Favata Comments: 26 pages, 7 figures Neskol'ko let nazad gruppa teoretikov predstavila raschety, soglasno kotorym pri sliyanii dvuh neitronnyh zvezd voznikalo interesnoe yavlenie. Pod deistviem prilivnyh sil plotnost' v centre neitronnoi zvezdy vozrastala, v rezul'tate chego ona kollapsirovala v chernuyu dyru. Rezul'taty byli, chto nazyvaetsya, kontrintuitivny, poetomu oni srazu zhe podverglis' zhestkoi kritike. Byla obnaruzhena oshibka v raschetah. Avtory soglasilis' s kritikoi i povtorili raschet. Kollaps bol'she ne poyavlyalsya, odnako nekotoroe uvelichenie plotnosti vse ravno nablyudalos' v modelyah. Poslednii fakt spodvig avtora nastoyashei stat'i rassmotret' bolee obshuyu zadachu o vozmozhnom szhatii neitronnoi zvezdy v processe sliyaniya. Dannoe issledovanie pokazalo, chto v chislennom raschete vse-taki mozhet vozniknut' situaciya, kogda kollaps proizoidet. Dlya etogo neitronnaya zvezda dolzhna obladat' kvadrupol'nym momentom. Odnako avtor ne isklyuchaet togo, chto effekt yavlyaetsya artefaktom chislennoi realizacii. astro-ph/0510684 Anizotropnoe teplovoe izluchenie zamagnichennyh neitronnyh zvezd (Anisotropic thermal emission from magnetized neutron stars) Authors: J.F. Perez-Azorin, J.A. Miralles, J.A. Pons Comments: 18 pages, 20 figures, submitted to A&A V poslednee vremya poyavilos' mnogo novyh interesnyh dannyh po teplovomu izlucheniyu neitronnyh zvezd. V pervuyu ochered' eto svyazano s ob'ektami, sostavlyayushimi Velikolepnuyu semerku. Estestvenno, chto s detalizaciei dannyh prihoditsya stroit' bolee slozhnye modeli, kotorye mogli by opisat' novye nablyudeniya. V etoi stat'e avtory rassmatrivayut anizotropiyu teplovogo izlucheniya neitronnyh zvezd, voznikayushuyu za schet sil'nogo magnitnogo polya. Postroennye modeli udovletvoritel'no opisyvayut nablyudatel'nye dannye. T.o., nablyudeniya izlucheniya mogut pomoch' opredelit' raspredelenie magnitnogo polya vnutri neitronnyh zvezd. astro-ph/0510687 Novyi mehanizm vzryvov sverhnovyh (A New Mechanism for Core-Collapse Supernova Explosions) Authors: Adam Burrows et al. Comments: 19 pages, including nine figures (in emulateapj format), submitted to the Astrophysical Journal Za nedostatkom vremeni ne budem podrobno razbirat' stat'yu. Otmetim tol'ko, chto rech' idet o roli akusticheskih voln v sbrose obolochki. Avtory pokazyvayut, chto posle stadii otskoka (bounce) akkreciruyushaya neitronnaya zvezda (chast' veshestva vsegda vypadaet obratno) yavlyaetsya samovozbuzhdayushimsya oscillyatorom. Generiruemoi energii hvataet dlya vzryva. Vydelenie energii asimmetrichno. astro-ph/0510693 Postroenie teplovoi i magnitnoi karty poverhnosti neitronnoi zvezdy po ee rentgenovskomu izlucheniyu: metod i analiz krivyh bleska (Unveiling the thermal and magnetic map of neutron star surfaces though their X-ray emission: method and lightcurves analysis) Authors: Silvia Zane, Roberto Turolla Comments: 17 pages, 9 figures. Figures 3 and 5 (top panel) are provided separately as .png files. Accepted for publication in MNRAS Rabota tesno primykaet k stat'e astro-ph/0510684. Avtory takzhe rassmatrivayut teplovoe izluchenie ob'ektov Velikolepnoi semerki. Avtory pytayutsya dat' udovletvoritel'noe opisanie dlya nablyudaemyh variacii spektra istochnika RX J0720.4-3125. Dlya etogo k dipol'nomu polyu dobavlena kvadrupol'naya komponenta. Pokazano, chto eto razumnaya ideya. T.e. opisat' zaregistrirovannye izmeneniya v izluchenii etogo istochnika nevozmozhno bez privlecheniya vysshih mul'tipolei. My budem starat'sya hotya by perechislit' interesnye (dlya shirokoi publiki) stat'i, poyavivshiesya v razdele physics (vklyuchaya cross-listing). physics/0510142 Global'noe povedenie indeksa produktivnosti issledovatelei (Universal Behavior of a Research Productivity Index) Authors: Pablo Diniz Batista et al. Comments: 5 pages, 1 figure and supplementary material Ocherednaya zametka, posvyashennaya sovershenstvovaniyu indeksa citirovaniya. Poskol'ku eta tema mne interesna, to, navernoe, ya budu upominat' obo vseh stat'yah na etu temu. Avtory pytayutsya uchest' kolichestvo soavtorov rabot. Vvoditsya modificirovannyi indeks hI=h/[Na], gde [Na]= N(T)a/h - srednee chislo soavtorov v h stat'yah. h - indeks, vvedennyi Hirshem ( ya o nem rasskazval). N(T)a - polnoe chislo soavtorov v h stat'yah (esli soavtor poyavlyaetsya neskol'ko raz, to on stol'ko raz i uchityvaetsya). T.o. hI=h2/N(T)a. Zamet'te, chto vazhno tol'ko chislo soavtorov v teh h stat'yah, kotorye i formiruyut indeks! T.e. mozhno pisat' skol' ugodno mnogo malocitiruemyh rabot v odinochku, no, esli samye citiruemye napisany s bol'shim chislom soavtorov, to eto skazhetsya na indekse hI. V stat'e privedeny dannye po vedushim fizikam. Vitten, kak byl na pervom meste, tak i ostaetsya, a vot dal'she est' nekotorye perestanovki. Krome togo, shkala rastyagivaetsya. Est' dlya Vittena h=110, a dlya stoyashego na desyatom meste Dzhona Bakala (Bahcall) h=76, to hI dlya Vittena raven 65.05, a dlya stoyashego na desyatom meste Kardony (Cardona) hI=6.21 (Bakal peremestilsya na 7-e mesto s hI =20.33). Krome togo, provedeno issledovanie na baze dannyh po brazil'skim uchenym (avtory brazil'cy - im i brazil'skii flag v ruki). Otdel'no hochu vyskazat' odnu mysl', napryamuyu svyazannuyu s ocenkoi citiruemosti. V nedavnei redakcionnoi stat'e v Nature (N7045, pp. 1003-1004 (2005)) byl podnyat vopros o roli nebol'shogo chisla aktivno citiruemyh statei: oni vnosyat bol'shoi vklad v impakt-faktor konkretnogo zhurnala. Predstavlyaetsya interesnym primenit' metodiku, predlozhennuyu Hirshem, ne tol'ko dlya ocenki vklada otdel'nogo uchenogo, no i dlya rascheta impakt-faktora. Sootvetstvenno, k etim raschetam mozhno primenyat' i nekotorye modifikacii h-indeks (razumeetsya, ne tu, chto obsuzhdaetsya v stat'e brazil'skih avtorov). Mozhno primenit' Hirshevu metodiku k zhurnalam, kogda budet ocenivat'sya ne srednee kolichestvo citirovanii na stat'yu, a nechto drugoe. Raznye varianty vozmozhny (odnako pochti navernyaka pridetsya delit' na kolichestvo statei, ili rasschityvat' na tysyachu, plyus nado uchityvat' faktor vremeni, chtoby starye zhurnaly ne imeli preimushestva pered molodymi, no uspeshnymi). Esli primenyat' metodiku "v lob", to dlya Nature poluchitsya chto-nibud' poryadka 1000 (tysyacha statei s indeksom citirovaniya vyshe 1000), a dlya AZh, skazhem 100 (sto statei s indeksom citirovaniya vyshe 100). Potom mozhno delit' eto na chislo statei, na vremya sushestvovaniya zhurnala. Mozhno chislo citirovanii dlya kazhdoi stat'i delit' na vremya s momenta ee publikacii (togda, konechno, ne nado bol'she nikak uchityvat' faktor vremeni - tol'ko chislo publikacii). Mozhno prosto rasschityvat' indeks za poslednie neskol'ko let. V obshem, vidno, chto metodika mozhet srabotat'. Interesno, kto-nibud' sdelaet stat'yu s takoi ideei? Zhalko, chto u nas nedostupna sistema ISI. P.S. Kak mne lyubezno soobshil sam professor Hirsh, on provodil nekotorye ocenki. Naprimer, dlya Solid State Communications h=147. a dlya Physics Letters A h=125. Kstati, bylo by takzhe interesno ocenivat' h-indeks dlya institutov. physics/0510188 Matematika, materiya i myshlenie (On Math, Matter and Mind) Authors: Piet Hut, Mark Alford, Max Tegmark Comments: 15 pages with figures Vsem sovetuyu hotya by prosmotret'. Tri izvestnyh issledovatelya rassuzhdayut o triade Menrouza (math. matter, mind). Rech' idet filosofskih osnovah nauki. Vernut'sya k nachalu stranicy

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