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L'asteroide Nea 2012 ASTRONOMIA NOVA L. Franco, P. Bacci, 2012 EG5 Pagina 54 n. 13, maggio 2012 L’ASTEROIDE NEA 2012 EG5 Lorenzo Franco e Paolo Bacci L‘Osservatorio astronomico di San Marcello Pistoiese L'asteroide NEA (Near Earth Asteroid, http:// Simone Vergari, nei giorni 21, 27 e 30 marzo. In parti- it.wikipedia.org/wiki/Oggetto_near-Earth ) 2012 EG5 è colare in quest'ultima data sono state effettuate alcune stato scoperto il 13 marzo 2012 dal telescopio Pan- sessioni osservative finalizzate alla fotometria per cerca- STARRS 1, Haleakala nelle Hawaii. Si tratta di un aste- re di determinare il periodo di rotazione dell'oggetto. roide di tipo Apollo (http://it.wikipedia.org/wiki/ Nel corso della sessione osservativa del 30 Marzo sono Asteroide_Apollo), con un diametro inferiore ai 100 state acquisite un totale di 479 immagini non filtrate da metri, che al momento della scoperta si trovava a circa 15 secondi di esposizione su un intervallo temporale di 36 volte la distanza Terra-Luna. L'asteroide è stato su- 2.5 ore. Tutte le immagini sono state riprese con il tele- bito classificato come un potenziale impattore virtuale scopio principale da 0.6 m ed una camera CCD Apogee dal JPL Sentry e dal NEODyS di Pisa. Le osservazioni Alta 1024 x 1024 con un campo di vista di 35x35 minuti astrometriche pervenute al Minor Planet Center nei d'arco ed un campionamento di 2 secondi d'arco per giorni successivi hanno permesso di determinare con pixel. Nonostante l'ampio campo inquadrato è stato ne- maggiore precisione l'orbita, scongiurando così ogni cessario spostare più volte l'inquadratura per seguire immediata possibilità di impatto. L'asteroide sarebbe l'oggetto che si muoveva velocemente (Fig. 2). comunque passato molto vicino alla Terra il 1° Aprile, Le immagini calibrate (con dark e flat) sono state analiz- ad una distanza di poco superiore alla metà della di- zate nei giorni successivi da Lorenzo Franco con MPO stanza Terra-Luna (Fig. 1); infatti il 4 aprile era stata Canopus (Fig. 3). L'analisi dei dati fotometrici, nono- programmata la sua osservazione radar attraverso il stante il basso segnale rumore dovuto al breve tempo di radiotelescopio di Goldstone, ma purtroppo senza alcun esposizione ed alla bassa luminosità dell'asteroide, han- risultato. L'asteroide è stato osservato con il telescopio no permesso comunque di determinare con buona preci- dell'osservatorio di San Marcello Pistoiese - MPC 104 sione un periodo di rotazione molto veloce di P = 0.2924 da Paolo Bacci, Luciano Tesi, Giancarlo Fagioli, ± 0.0002 h (poco più di 17 minuti). L. Franco, P. Bacci, 2012 EG5 ASTRONOMIA NOVA n. 13, maggio 2012 Pagina 55 Fig. 1. Il Period Spectrum (Fig. 4) mostra il risultato della ricerca del periodo, dove il valore più probabile corri- sponde a quello con l'errore RMS più basso. Il grafico in Fig. 5 mostra la curva di luce completa ottenuta dalle tre ses- sioni osservative messe in fase. L'ampiezza della variazione lumino- sa è risultata di 0.42 ± 0.01 mag. Il risultato originale ottenuto da questo lavoro è stato sottomesso per la pubblicazione sul prossimo nu- mero del Minor Planet Bulletin. Fig. 2. La traccia lascia- ta dall'asteroide durante il suo veloce movimento Fig. 3. La sessione fotometrica con MPO Canopus. In primo piano il tool Comp Star Selector che permette di scegliere le stelle di confronto, selezionan- dole tra quelle con co- lore simile a quello Solare. ASTRONOMIA NOVA L. Franco, P. Bacci, 2012 EG5 Pagina 56 n. 13, maggio 2012 Fig. 5. Curva di fase che mostra due massimi e due mi- Fig. 4. Il grafico mostra il risultato della ricerca del periodo. Il valore più probabile è quello con l'errore RMS più basso. nimi di profondità diversa. L'ampiezza della curva di luce A = 0.42 ± 0.01 magnitudini. Una raffigurazione artistica dell‘asteroide 2012 EG5. Paolo Bacci, nato nel 1968, astrofilo sin dall'adolescenza, Lorenzo Franco, nato a Monte S. Angelo (FG), è appassio- quando si associò al GAMP Gruppo Astrofili Montagna Pisto- nato di Astronomia da sempre, tanto da conseguire la Lau- iese, e si occupava dell'osservazione visuale di meteore e stelle rea in Astronomia presso l'Università di Bologna. Vive e la- variabili. Successivamente è entrato a far parte dell'AAAV vora a Roma nel settore dell' Information Tecnology di una Associazione Astrofili Alta Valdera, dove si occupa di asteroidi Banca. Dal 2005 si dedica nel tempo libero all'osservazione e comete. Osserva da: Capannoli (PI), Osservatorio ―G. Gali- di asteroidi e comete ed alla ricerca scientifica amatoriale, lei‖ Centro Astronomico Libbiano Peccioli (PI), San Marcello collabora con la Sezione Stelle Variabili dell'UAI. Pistoiese (PT). Il suo sito www. backman.altervista.org L. Franco, Fotometria ASTRONOMIA NOVA n. 13, maggio 2012 Pagina 57 FOTOMETRIA DI ASTEROIDI E STELLE VARIABILI Un’invito all’osservazione Lorenzo Franco Asteroide 1269 Rollandia 1269 Rollandia è un asteroide di fascia principale, sco- perto il 20 settembre 1930 da G. Neujmin a Simeis in Crimea (Ucraina), con un diametro di circa 100 km. Le sue principali caratteristiche sono consultabili sul sito JPL Small-Body Database Browser all'indirizzo: http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=rollandia&orb=1 L'asteroide è stato osservato da A. Ferrero, L. Franco e R. Zambelli in sei diverse sessioni osservative che han- no permesso di ottenere una prima stima del periodo di rotazione P = 16.40 +/- 0.01h con un' ampiezza della curva di luce A = 0.05 mag. Sarebbe necessaria qualche Stelle Variabili altra sessione osservativa per poter confermare con A maggio sono osservabili le seguenti stelle variabili maggiore certezza il periodo di rotazione. pulsanti, che rientrano anche nel programma osservati- Vi invito pertanto ad osservare 1269 vo della sezione stelle variabili SSV-UAI-GRAV. Rollandia! La tecnica osservativa è ampiamente descritta nel mio RS Boo (fig. 1) articolo: http://www.eanweb.com/2012/fotometria- Variabile pulsante di magnitudine: 9.69 - 10.84 V con delle-stelle-variabili-come-si-realizza-una-curva-di- un periodo di 0.3773 d (circa 9.06 h). luce/ La cartina di riferimento e la magnitudine delle stelle di confronto si trovano su: ASTRONOMIA NOVA L. Franco, Fotometria Pagina 58 n. 13, maggio 2012 ST Boo (fig. 4) variabile pulsante di magnitudine 10.49 - 11.41 V con un periodo di 0.6223 d (circa 14.9 h). La cartina di riferimento e la magnitudine delle stelle di confronto si trovano su: http://stellevariabili.uai.it/images/6/6e/ ST_Boo_E_chart.png http://stellevariabili.uai.it/images/9/94/ ST_Boo_field_photometry.pdf Fig. 1. Curva di luce di RS Boo, in ascissa la fase. Il grafico è tratto da: A. Nagy, “Studies on amplitude modulated RR Lyrae Stars. II. RS Bootes”, http://adsabs.harvard.edu/ abs/1998A%26A...339..440N http://stellevariabili.uai.it/images/2/29/ RS_Boo_E_chart.png http://stellevariabili.uai.it/images/e/e5/ RS_Boo_field_photometry.pdf SW Boo (fig. 2) variabile pulsante di magnitudine 11.76 - 12.88 V con un periodo di 0.5135 d (circa 12.3 h). La cartina di riferimento e la magnitudine delle stelle di confronto si trovano su: Fig. 3. Osservazione di un periodo principale di TV Boo, dal http://stellevariabili.uai.it/images/f/fe/ sito: http://www.univie.ac.at/tops/blazhko/Winter.html SW_Boo_E_chart.png http://stellevariabili.uai.it/images/1/1c/ SW_Boo_field_photometry.pdf TV Boo (fig. 3) variabile pulsante di magnitudine 10.71 - 11.30 V con un periodo di 0.3126 d (circa 7.5 h). La cartina di riferimento e la magnitudine delle stelle di confronto si trovano su: http://stellevariabili.uai.it/images/8/80/ TV_Boo_E_chart.png http://stellevariabili.uai.it/images/b/b3/ Fig. 4. Curva di luce di ST Boo, tratta da: http:// TV_Boo_field_photometry.pdf adsabs.harvard.edu/abs/1993A%26AS..101..195P Fig. 2. Curva di luce di SW Boo, ottenuta da A.D. Bonov a Budapest nel 1955, http:// adsabs.harvard.edu/ abs/1955CoKon..38....1B .
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