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Follow-Up Di Tnos Follow-up di TNOs ell’ambito dell’attività di ricerca dei corpi Principalmente sono ricoperti da ghiaccio, si Paolo Bacci minori del sistema solare – asteroide e co- presuppone che conservino nella loro struttura i GAMP Nmete – si soci del GAMP Gruppo Astro li fossili della nube proto-stellare che ha formato Gruppo Astro li Montagna Montagna Pistoiese, che gestiscono l’osservatorio il nostro sistema solare. Pistoiese della Montagna Pistoiese, struttura pubblica del Dall'analisi spettroscopica sono composti ge- Osservatorio Astronomico comune di San Marcello Pistoiese, hanno effet- neralmente da una miscela di idrocarburi leggeri: della Montagna Pistoiese tuato il follow-up dell’asteroide 2008 CT190, metano, ammoniaca e ghiaccio d'acqua, molto www.gamp-pt.net TNOs (Trans-Neptunian Object), simili alla composizione delle comete. I TNOs hanno un orbita oltre le 30 Unità Il primo ad essere stato scoperto è Pluto nel astronomiche, ovvero oltre l’orbita di Pluto, co- 1930, i più grandi corpi conosciuti appartenenti nosciuti anche come KBO (Kupier Belt Object), a questa categoria sono: Eris, Makemake, 2007 rappresentano la nuova frontiera del nostro siste- OR10 e Haumea, le cui dimensioni sono di circa ma solare. La popolazione dei TNOs è composta 1500 km. da circa 1490 oggetti. (http://www.minorpla- Essendo corpi molto distanti il loro studio è Figura 1. TNOs distanza dal sole e netcenter.net/iau/lists/TNOs.html) particolarmente dif coltoso. Grazie al recente dimensioni. Unione Astrofi li Italiani>www.uai.it ASTRONOMIA 29 Esperienze, divulgazione e didattica Figura 2. Rappresentazione delle dimensioni dei TNOs. Figura 4. Diagramma semiasse maggiore (a) Vs Inclinazione( Incl.). passaggio ravvicinato della sonda New Horizons della NASA con Pluto si hanno maggiori informazioni e dati su questi corpi freddi e remoti. I KBOs essendo molto distanti dal Sole sono in uenzati dalle forze gravitazionale dei pianeti giganti ed in particolare modo da Nettuno alle risonanze orbitali 2:3 e 1:2. In questa zona di spazio vi sono due principali categorie di oggetti, quelli che orbitano intorno al Sole con un eccentricità prossima allo zero (come la maggior parte dei pianeti del sistema solare) ed gli altri con un eccentricità oltre 0.3 e inclinazione superiore ai 30°. Di seguito si riportano in gra co la distanza del semiasse mag- giore (a ) e la distanza perielica (q), che evidenzia una distribuzione non omogenea dei TNOs. La distribuzione dei KBOs in funzione della distanza dal Sole mostra una “lacuna” intorno a 48 UA. Secondo alcuni astronomi, come Alan Stern e Patryk Lykawka, la causa potrebbe essere l’in- terazione gravitazionale di un oggetto di massa planetaria ancora Figura 5. Semiasse Maggiore (a ) vs Perielio (q). sconosciuto, della taglia di Marte o della Terra, oppure secondo Figura 3. Immagine della super cie di Pluto ripresa dalla sonda New Horizons (NASA). Figura 5. Semiasse Maggiore (a ) vs Perielio (q). 30 ASTRONOMIA n. 4 • luglio-agosto 2016 Esperienze, divulgazione e didattica altri dovuto alla presenza di un oggetto più massiccio posto a In base ai dati conosciuti veniva lanciata una sequenza di circa 1500 UA. I TNOs, come detto essendo molto lontani dal Sole hanno un periodo siderale di centinaia di anni, per cui il loro moto apparente sulla volta celeste risulta, di norma, molto lento. Questa regione, la c.d. Fascia di Kupier, ha un esenzione da 30 UA no a 50 UA, e si pensa sia il bacino delle comete a corto periodo. E’ una zona ancora inesplorata e che in futuro potrà dare importanti indicazioni sulla formazione del nostro sistema solare. L’asteroide 2008 CT190, TNOs, è stato scoperto la notte del 9 febbraio 2008 dall’ osservatorio di Palomar Mountain (MPC 675) utilizzando il telescopio da 1.2-m in con gurazione Oschin Schmidt, dagli astronomi: M. E. Schwamb, M. E. Brown, D. Rabinowitz. Dal sito Astdys2 (http://hamilton.dm.unipi.it/astdys/index. php?pc=1.1.7.0&n=2008%20CT190) risultano solo 42 osserva- Figura 7. Orbita dell’asteroide 2008 CT190. zioni, di cui 8 pre-scoperta, l’ultima risale al 10 marzo del 2013. Elementi orbitali Epoch 2016 July 31.0 TT = JDT 2457600.5 MPC immagini ognuna da 60 secondi, per un totale di 30 immagini. Al M 4.13700 (2000.0) P Q ne di poter apprezzare lo spostamento dell’asteroide nelle nostre n 0.00253572 Peri. 48.03203 -0.72055580 -0.33045087 T = immagini, abbiamo ripreso la stessa zona di cielo dopo circa 3,7 2455969.01043 JDT ore, riuscendo cosi a notare il movimento dell’asteroide che, dalle a 53.2601068 Node 103.65942 +0.28519259 -0.94257195 nostre misure, è risultato avere una magnitudine di ~20,8. q = 34.6981429 Dopo accurati controlli le nostre misure astrometriche sono e 0.3485153 Incl. 38.85374 +0.63203206 +0.04858337 state inviate al Minor Planet Center. In g. 8 viene indicata la zona P 389 H 5.5 G 0.15 U1 di cielo ripresa, con evidenziato l’asteroide 2008 CT190, ripreso From 45 observations at 9 oppositions, 2002-2016, mean residual 0”.37. dell’osservatorio astronomico di San Marcello. Inoltre, abbiamo trasmesso le nostre misure astrometriche La sera del 6 maggio 2016 il team di astro li del GAMP guidati all’astronomo Fabrizio Bernardi, amministratore di SpaceDys e da Paolo Bacci, composto da Luca Nerli, Martina Maestripieri e gestore del sito Neodys e AstDys, il quale ha calcolato i residui Leonardo Mazzei, utilizzando il telescopio da 0,60-m F/4 , munito delle nostre misure, confermando la buona qualità da noi ottenuta. di CCD 1024x1024, con FOV di 35’x35’ e risoluzione 2”/pixel, ( Per i soci del GAMP è stata davvero una bella esperienza e Codice MPC 104 San Marcello), hanno puntato la zona di cielo dove motivo di grande soddisfazione effettuare il follow-up di un aste- era previsto la presenza dell’asteroide 2008 CT190. Dalle effemeridi roide TNOs la cui luminosità era al limite delle potenzialità del del Minor Planet Center risultava una luminosità di 21.0 mag, con nostro strumento, riuscendo a misurare un asteroide che si trovava un motion di 0,03”/min e PA 220; trovandosi ad una distanza dal ad una distanza di oltre 5 miliardi di km le cui dimensioni sono Sole di 34 8 UA ( circa 5.206.080.000 km). stimate in 350 km. Figura 8. L’asteroide 2008 CT190 ripreso dall’Osservatorio di San Marcello Pistoiese. Unione Astrofi li Italiani>www.uai.it ASTRONOMIA 31 Esperienze, divulgazione e didattica Osservazioni dell’asteroide TNOs 2008 CT190 presenti nel database del MPC 2002 02 08.25931 08 52 32.98 +35 44 44.6 20.1 r 705 – Apache Point MPS 449646 2002 02 08.26014 08 52 32.98 +35 44 44.7 705 – Apache Point MPS 449646 2002 02 08.26263 08 52 32.95 +35 44 44.7 705 – Apache Point MPS 449646 2002 02 12.35304 08 52 05.96 +35 46 37.0 21 R 644 – Palomar Mountain/NEAT MPS 387243 2002 02 12.39759 08 52 05.66 +35 46 38.1 644 – Palomar Mountain/NEAT MPS 387243 2002 11 07.454006 09 08 11.76 +35 13 28.8 21.1 V 645 – Apache Point-Sloan Digital Sky Survey MPS 604621 2002 11 07.454835 09 08 11.76 +35 13 28.8 20.8 V 645 – Apache Point-Sloan Digital Sky Survey MPS 604621 2002 11 07.457323 09 08 11.77 +35 13 28.9 21.6 V 645 – Apache Point-Sloan Digital Sky Survey MPS 604621 2008 02 09.48728 09 52 54.32 +38 53 04.1 21.1 R 675 – Palomar Mountain MPS 249836 2008 02 09.53457 09 52 53.98 +38 53 05.3 21.0 R 675 – Palomar Mountain MPS 249836 2008 02 10.35833 09 52 48.43 +38 53 39.3 21.5 R 675 – Palomar Mountain MPS 249836 2008 02 10.40611 09 52 48.16 +38 53 41.0 21.3 R 675 – Palomar Mountain MPS 249836 2008 02 27.15774 09 50 54.76 +39 02 55.5 688 – Lowell Observatory, Anderson Mesa Station MPS 249836 2008 02 27.24540 09 50 54.16 +39 02 57.5 688 – Lowell Observatory, Anderson Mesa Station MPS 249836 2008 03 12.14846 09 49 26.22 +39 07 22.4 675 – Palomar Mountain MPS 249836 2008 03 12.29903 09 49 25.29 +39 07 24.1 675 – Palomar Mountain MPS 249836 2008 03 12.36855 09 49 24.88 +39 07 25.1 675 – Palomar Mountain MPS 249836 2008 04 02.20838 09 47 40.30 +39 08 03.1 675 – Palomar Mountain MPS 249836 2008 05 03.24090 09 46 35.56 +38 57 08.6 675 – Palomar Mountain MPS 249836 2008 05 04.21209 09 46 35.56 +38 56 36.8 675 – Palomar Mountain MPS 249836 2008 10 25.45330 10 06 19.32 +37 41 32.0 695 – Kitt Peak MPS 265296 2008 10 25.48941 10 06 19.50 +37 41 33.1 695 – Kitt Peak MPS 265296 2008 10 27.40825 10 06 29.31 +37 42 29.7 695 – Kitt Peak MPS 265296 2008 10 27.44105 10 06 29.46 +37 42 30.4 695 – Kitt Peak MPS 265296 2009 02 26.32375 10 01 31.86 +39 23 40.2 20.5 R 688 – Lowell Observatory, Anderson Mesa Station MPS 278751 2009 02 26.36956 10 01 31.56 +39 23 41.5 688 – Lowell Observatory, Anderson Mesa Station MPS 278751 2009 03 12.13214 10 00 02.87 +39 28 31.1 675 – Palomar Mountain MPS 281350 2009 03 13.24076 09 59 56.08 +39 28 46.1 675 – Palomar Mountain MPS 281350 2009 03 24.19264 09 58 54.38 +39 30 08.7 20.7 R 688 – Lowell Observatory, Anderson Mesa Station MPS 281350 2009 03 24.24475 09 58 54.09 +39 30 08.9 688 – Lowell Observatory, Anderson Mesa Station MPS 281350 2009 03 25.18686 09 58 49.26 +39 30 10.2 688 – Lowell Observatory, Anderson Mesa Station MPS 281350 2009 03 25.27341 09 58 48.81 +39 30 10.3 688 – Lowell Observatory, Anderson Mesa Station MPS 281350 2010 03 09.86696 10 11 00.78 +39 45 25.8 20.5 V A74 – Bergen-Enkheim Observatory MPS 316783 2010 03 09.90745 10 11 00.55 +39 45 26.5 20.9 V A74 – Bergen-Enkheim Observatory MPS 316783 2010 03 09.92287 10 11 00.49 +39 45 26.8 20.8 V A74 – Bergen-Enkheim Observatory MPS 316783 2011 01 10.46484 10 27 47.15 +39 14 14.2 20.6 R 695 – Kitt Peak MPS 375601 2011 01 10.51359 10 27 46.95 +39 14 17.5 695 – Kitt Peak MPS 375601 2011 01 10.55114 10 27 46.75 +39 14 19.2 695 – Kitt Peak MPS 375601 2011 12 26.41367 10 39 17.02 +39 05 43.5 20.6 R 688 – Lowell Observatory, Anderson Mesa Station MPS 404710 2011 12 26.48007 10 39 16.88 +39 05 47.9 688 – Lowell Observatory, Anderson Mesa Station MPS 404710 2013 03 10.06371 10 43 35.17 +40 15 39.8 I17 – Thomas G.
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