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Unlink or relink any files in which the filename is preceded with a question mark or other symbol. For more information about In. Design links, see Managing graphics links. Sometimes errors are a result of a particular function in the print or export process, as it is handling some specific content in the document. Eliminate as many of these types of settings as possible. If eliminating settings resolves the issue, enable them again in groups to isolate the problem to a particular setting. Note: Depending on which printer you're using, some of the settings may be unavailable. Choose File > Print to open the Print dialog box. Then change the following settings in the following panes: Set copies to 1. Select Pages to disable Spreads. Clear Print Master Pages, Print Non- printing Objects,and Print Visible Guides and Baseline Grids. Set print layers to Visible & Printable Layers. Set paper size to Defined by Driver. Set scale width and height to 1. Disable Thumbnails and Tile. Disable Marks, Bleed,and Slug. Set color to Composite Leave Unchanged. Disable Trapping, Text as Black, and Simulate Overprint. In the Ink Manager, disable Ink Aliasing. Set images to Send Data to None or All. Set fonts to Download to None or All. Set Post. Script to Level 2. Set data format to ASCII. Set color handling to Let Post. Script Printer Determine Colors. Enable Preserve CMYK Numbers. Select all the pages, right- click, and then choose Page Attributes > Spread Flattening > None (Ignore Transparency). Remove third- party plug- ins from the In. Design Plug- ins folder, and then restart In. Design. If the problem recurs, move the plug- ins back to the In. Design Plug- ins folder. If the problem doesn't recur, identify conflicting plug- ins: Choose Help > Configure Plug- Ins (Windows) or In. Design > Configure Plug- Ins (Mac OS). Select All Plug- Ins for the Set and then clear all the options in the Display section except Third Party. Create a list of these plug- ins. Quit In. Design and move these plug- ins out of the Plug- in folder: Windows: /Program Files/Adobe/Adobe In. Design . Create a new user account (don't delete your original one), log in to the new account, and try to print or export the document again. Choose Start > Control Panel > User Accounts. Choose Apple menu > System Preferences > Users & Groups. See Troubleshoot damaged In. Design documents. If you receive an error when printing any In. Design document, try one or more of the following tasks to identify the cause of an application- level problem. When In. Design is behaving erratically, deleting preferences (also referred to as “trashing preferences” or “removing preferences”) and re- creating them often solves the problem. There are two ways to re- create preferences: Automatically: This method quickly deletes your current preference files and then regenerates a new set of default preference files. However, any custom settings you may have had are lost.- or- Manually: If you don't want to lose your custom settings, rename your current preference files before regenerating a new set of default preference files. That way, if new preferences don't solve your print or export problem, you have a backup of your original preference files (including any custom settings), which you can use to replace the new preference files. Quit In. Design. Relaunch In. Design and immediately hold down the appropriate keys for your OS: Mac OS: Control+Option+Command+Shift. Windows: Control+Alt+Shift. A dialog box appears, asking if you want to delete In. Design preference files. In. Design launches with regenerated default preferences. Rename the two preference files (e. The preference files are located here: Mac OS XIn. Design Defaults: Users/. Learn how to show hidden files. In. Design Saved. Data: /Documents and Settings/. Learn how to show hidden files. In. Design Saved. Data: /Users/. In. Design creates a new set of default preference files. If your print or export problem persists, then you can restore your original preferences by renaming your old preference files back to their original names: In. Design Saved. Data and In. Design Defaults. Install the most recent driver for your printer: Choose File > Print. Click Setup, select a printer, click Preferences, and then click Advanced. Expand Document Options, and then expand Post. Script Options. Choose Post. Script Output Option. Choose Optimize for Speed from the pop- up menu, and then click OK. Click OK and then click Print. See the documentation included with the printer for instructions on how to disable this feature. If the problem occurs when you print over a network, connect the computer directly to the printer and try printing again. If you can't connect directly to the printer, save the document as a Post. Script file. 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Uno degli esperimenti a bordo del Compton era il Burst & Transient Source Experiment (BATSE), che poteva rilevare lampi di raggi gamma e localizzare le loro posizioni nel cielo con ragionevole precisione. Se infatti fossero eventi che avvengono nella nostra galassia allora sarebbero distribuiti preferibilmente sul piano della Via Lattea; anche se fossero associati con l'alone galattico, sarebbero distribuiti soprattutto verso il centro galattico, a meno che le dimensioni dell'alone non siano enormemente maggiori di quanto stimato. Inoltre le galassie vicine avrebbero dovuto presentare aloni simili, ma non misero in risalto “macchie di luce” di deboli lampi di raggi gamma. I lampi corti durano tipicamente meno di due secondi e le emissioni sono dominate da fotoni ad alta energia; i lampi lunghi durano tipicamente pi. La separazione tra le due categorie non . La migliore speranza di cambiare questa situazione sembrava risiedere nella possibilit. Dopo aver rivelato un gamma- ray burst (GRB 9. Ulteriori osservazioni con telescopi a terra identificarono una debole controparte ottica. Con la posizione della sorgente perfettamente nota, quando l'emissione di raggi gamma si affievol. Entro poche settimane, la controversia sulle distanze di questi eventi aveva raggiunto una conclusione: i lampi gamma potevano essere finalmente identificati come eventi extra- galattici, che si originavano in galassie molto deboli. Questa scoperta rivoluzion. Il satellite Swift combina un rilevatore di raggi gamma molto sensibile con la capacit. La gamma di teorie proposte per spiegare i GRB prevedevano locazioni assai diverse del fenomeno, dalle regioni esterne del nostro sistema solare ai limiti estremi dell'universo conosciuto. La scoperta che tali esplosioni erano isotrope diminu. Nel loro modello postulavano che esistesse una popolazione finora non osservata di oggetti analoghi ad una distanza maggiore che originava i gamma- ray burst. Inoltre, ritenevano eccessivo il quantitativo di energia richiesto a generare un tipico lampo gamma se si fosse ammessa l'ipotesi che avvenissero in una galassia distante. I ricercatori che sostenevano il modello extra- galattico. Tuttavia, oggi sappiamo che i lampi di raggi gamma non sono semplicemente eventi extra- galattici, ma che avvengono praticamente al limite dell'universo visibile. Un GRB tipico ha un redshift non inferiore a 1. Tuttavia, le osservazioni permettono di acquisire lo spettro solo di una piccola frazione dei lampi gamma - generalmente di quelli pi. Se assumiamo che ogni lampo gamma emette energia uniformemente in tutte le direzioni, alcune tra le esplosioni pi. Tuttavia il requisito energetico . In molti lampi di raggi gamma si . Inoltre, almeno per una supernova, simile alle poche che sono state chiaramente identificate per aver accompagnato un gamma- ray burst, sono state osservate caratteristiche evocative di una significativa asimmetria nella sua esplosione (guarda . L'angolo di apertura del getto (grado di collimazione), comunque, sembra variare largamente da 2 gradi a pi. Ci sono alcune prove che l'angolo del getto possa essere correlato all'energia apparentemente rilasciata in modo che l'energia realmente rilasciata da un GRB (lungo) sia approssimativamente costante - circa 1. J, o approssimativamente 1/2. Questo valore . Infatti, sembra che luminose hypernovae abbiano accompagnato alcuni gamma- ray burst. Il fatto che i lampi di raggi gamma siano dei getti suggerisce che il numero di tali eventi nell'universo sia maggiore del valore che stimiamo dalle nostre osservazioni, anche tenendo conto del limite di sensibilit. Anche con queste considerazioni, il tasso di comparsa dei gamma- ray burst . Se il getto . Ma, anche i gamma- ray burst pi. I GRB corti, sebbene sempre extra- galattici, sembrano provenire da popolazioni a redshift inferiori e sono meno luminosi dei GRB lunghi. Inoltre appaiono generalmente meno collimati. Sono probabilmente pi. I lampi di raggi gamma stessi mostravano una grande variet. Si teorizza che progenitori dei GRB lunghi siano dovuti al collasso dei nuclei di stelle massicce, a bassa metallicit. La stella rilascia energia nella forma di getti lungo l'asse di rotazione, generando un gamma ray burst. Fonte: Nicolle Rager Fuller/NSFC'. Quando una stella massiccia giunge alla sintesi del ferro, il processo di fusione nucleare assorbe pi. Nel caso la massa del nucleo superi un valore critico (2 o 3 masse solari), la contrazione conduce alla formazione di un buco nero. La materia della stella che non ha partecipato alla formazione del buco nero, continua a precipitare attratta da esso e (nel caso che la stella progenitrice avesse posseduto una grande velocit. Quando il materiale del disco cade nel buco nero si originano due getti lungo l'asse di rotazione (direzione di densit. Se la stella non . Il fronte d'onda accelera al decrescere della densit. Una volta raggiunta la superficie, l'onda d'urto erompe nello spazio, dove la maggior parte della sua energia . Sono necessarie ulteriori ricerche per affinare la teoria presentata ed identificare i valori limite della massa, velocit. Primo, gamma- ray bursts lunghi sono stati individuati in sistemi in cui . Altri modelli che prevedono un'associazione con la formazione stellare ne sono ugualmente favoriti. Secondo, sono stati osservati diversi casi in cui un'esplosione di supernova ha immediatamente seguito l'emissione del lampo gamma. Sebbene la maggior parte dei gamma- ray burst avvengano a distanze cos. Tali supernove sono state tutte classificate come del tipo Ib/c, una classe di rare supernove dovute al collasso del nucleo ma che mancano linee di assorbimento dell'idrogeno (consistentemente con l'associazione teorica con stelle che abbiano perso il loro involucro di idrogeno). Tra le associazione di GRB e supernove pi. Nonostante un'intensa attivit. Entrambi gli eventi sono stati comunque associati con popolazioni in cui . Una possibile implicazione . Ad oggi, sono state individuate le galassie ospiti solo per una manciata di eventi, che, inoltre, sembrano mostrare delle significative differenze dalla popolazione dei lampi lunghi: per quanto un lampo corto sia stato localizzato con precisione in una regione di formazione stellare, nella zona centrale di una galassia, molti altri sono stati associati con le regioni pi. Inoltre, tutti i GRB corti osservati finora hanno presentato un basso valore di redshift. Questa lista non tenta nemmeno di essere completa, includendo soltanto quei GRB che hanno un'importanza storica o scientifica. Il primo GRB rilevato. Il primo GRB di cui . Fu anche possibile individuare la provenienza dell'emissione da una galassia molto lontana (redshift z=0. Questa scoperta rafforz. Con z=0. 8. 35, conferm. Il GRB stesso fu molto inusuale, essendo estremamente poco luminoso. ISBN 8. 8- 2. 00- 3. EN) Meegan, C. A., et al. EN) Kouveliotou, C. L1. 01^(EN) Fishman, C. I gamma- ray burst sono designati dalla data di rilevazione: le prime due cifre della sigla indicano le ultime due cifre dell'anno, le due cifre successive indicano il mese, le ultime due cifre il giorno: AAMMDD (in inglese YYMMDD). Se sono rilevati pi. Inizialmente, non tutti i ricercatori accettarono l'attribuzione, e il redshift esatto della galassia in questione non fu ottenuto se non molti anni dopo. Comunque, il lampo gamma successivamente ben localizzato, GRB 9. Galassia senza alcuna ambiguit. EN) Paczynski, B. EN) Sari, R., Piran, T., Halpern, J. L1. 7- L2. 0^(EN) Frail, D. A. L5. 5- L5. 8^(EN) Galama, T. EN) Podsiadlowski et al. P^ab(EN) Prochaska et al. EN) Watson, D. GRB 0. Astronomy and Astrophysics, vol. L1. 23- L1. 26^(EN) Grupe, D. I: The Uncollimated Afterglow of GRB 0. Astrophysical Journal, in pubblicazione^(EN) Ruderman, M. EN) Mac. Fadyen, A. I.; Woosley, S. E.; Heger, A. EN) Blandford, R. D. 1. 13. 0- 1. 13. EN) Bloom, J. S., Kulkarni, S. R., & Djorgovski, S. EN) Sollerman, J. S^(EN) Mazzali, P. M^(EN) Kulkarni, S. R., et al. 6. 63^con riferimento ai tempi pi. |
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