DOCSLIB.ORG

Asteroid Lightcurves at the Palmer Divide Observatory Þ®·¿² É¿®²»®

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Asteroid Lightcurves at the Palmer Divide Observatory Þ®·¿² É¿®²»® Asteroid Lightcurves at the Palmer Divide Observatory Þ®·¿² É¿®²»® ̸» °®·³¿®§ ©±®µ ¿¬ ̸» п´³»® Ü·ª·¼» Ѿ•»®ª¿¬±®§ ·• ¬± ¼»¬»®³·²» ¬¸» ´·¹¸¬½«®ª» °¿®¿³»¬»®• ±º ¿• ³¿²§ ¿•¬»®±·¼• ¿• °±••·¾´»ò ̸·• ¹®±•• •«®ª»§ ³»¿²• ¬¸¿¬ ¿²§ ¹·ª»² ¿•¬»®±·¼ ·• ©±®µ»¼ ±²´§ «²¬·´ ¿ ®»¿•±²¿¾´§ ¿½½«®¿¬» •»¬ ±º °¿ó ®¿³»¬»®• ø°»®·±¼ ¬± ðòððëóðòðï¸ ¿²¼ ¿³°´·¬«¼» ðòðî³÷ ·• ¼»¬»®³·²»¼ º±® ¿ ¹·ª»² ´«²¿¬·±²ò Ô±²¹ ¬»®³ ¿²¿´§•·• ©·¬¸ ´±²¹»® ®«²• ¿²¼ñ±® •»ª»®¿´ ©»»µ• ·• ²±¬ °¿®¬ ±º ¬¸» ¹»²»®¿´ °®±¹®¿³ò Ѳ ±½½¿•·±²ô ³±®» ¼»¬¿·´»¼ ©±®µ ·• °»®º±®³»¼ ¿¬ ¬¸» ®»¯«»•¬ ±º ±¬¸»® ®»•»¿®½¸»• ¬¸¿¬ ¿®» ¿¬¬»³°¬·²¹ ¬± ®»º·²» ±® ®»³±ª» ¿³¾·¹«·¬§ º®±³ °®»ª·±«•´§ »•¬¿¾´·•¸»¼ °¿ó ®¿³»¬»®•ò ɸ§ ß•¬»®±·¼ Ô·¹¸¬½«®ª»•á Ü®ò ß´¿² Ø¿®®·• ±º ¬¸» Ö»¬ Ю±°«´•·±² Ô¿¾±®¿¬±®§ ¸¿• ¹·ª»² •»ª»®¿´ ¹±±¼ ®»¿•±²• º±® ¼±·²¹ ¿•¬»®±·¼• ´·¹¸¬½«®ª»• øØ¿®ó ®·• ó ïççè÷ •± ¬¸»®» • ²± ²»»¼ ¬± ¹·ª» ¿ ´±²¹ ´·•¬ ¸»®»ò ײ •¸±®¬ô ¬¸» •¬«¼§ ±º ¿•¬»®±·¼ ´·¹¸¬½«®ª»• ¬·»¼ ¬± ¬¸» ½´¿••·º·½ ¿ó ¬·±² ±º ¬¸» ¿•¬»®±·¼ ¾§ ±®¾·¬ô º¿³·´§ ¬·»•ô ¿²¼ ½±³°±•·¬·±² ½¿² ¸»´° ®»•±´ª» •»ª»®¿´ ·••«»• ½±²½»®²·²¹ ¬¸» ±®·¹ ·² ¿²¼ »ª±´«¬·±² ±º ¬¸» ³·²±® °´¿²»¬• ·²¼·ª·¼«¿´´§ ¿²¼ ¿• ¿ ©¸±´»ò ̱±ô ´·¹¸¬½«®ª» ±¾•»®ª¿¬·±²• º·®•¬ ´»¿¼ ¬± ¬¸» •«•°·½·±²ô ²±© ½±²º·®³»¼ô ±º ¿•¬»®±·¼• ¸¿ª·²¹ •³¿´´ •¿¬»´´·¬»• ±® ¼«¿´ó¾±¼·»¼ò ɸ¿¬ ·• ¾»½±³·²¹ ·³°±®¬¿²¬ ²±© ·• ¬¸» •»´»½¬·±² °®±½ó »••ò Ó±•¬ ±º ¬¸» ¾®·¹¸¬ô »¿•§ ¬¿®¹»¬• ¸¿ª» ¾»»² ¬¿µ»² ô ³»¿²·²¹ ³±•¬´§ ´¿®¹»® ³¿·²ó¾»´¬ ¿•¬»®±·¼•ò ׺ ¿¬ ¿´´ °±••·¾´»ô •¬«¼·»• •¸±«´¼ ¹·ª» •±³» °®·±®·¬§ ¬± ±¬¸»® ¬¿®¹»¬•ò Ò±¬ ¶«•¬ ÒÛÑ ¬¿®¹»¬• •¸±«´¼ ¾» ½±²•·¼»®»¼ô ¾«¬ ¬¸±•» ©·¬¸ ¸·¹¸´§ ·²½´·²»¼ ±® »½½»²¬®·½ ±®¾·¬• ¿• ©»´´ ¿• ¬¸» Ý»²¬¿«®• ¿²¼ ¾»§±²¼ò ̸» Û¯«·°³»²¬ ¿¬ ¬¸» п´³»® Ü·ª·¼» Ѿ•»®ª¿¬±®§ Ü«®·²¹ ïçççô ¿ îë½³ ÔÈóîðð ÍÝÌ ©¿• «•»¼ ¿´±²¹ ©·¬¸ »·¬¸»® ¿² ÍÞ×Ù ÍÌóéÛ ø»²¸¿²½»¼ ¾´«» ½¸·°÷ ±® ÍÌóè ø•¬¿²¼¿®¼ ½¸·°÷ò ̸» ½¿³»®¿ ©¿• ®«² ¿¬ óïð Ýô »ª»² ¬¸±«¹¸ ´±©»® ¬»³°»®¿¬«®»• ½±«´¼ ¾» ®»¿½¸»¼ ¼«®·²¹ º¿´´ ¿²¼ ©·²¬»®ò ̸·• ¿´´±©»¼ ¿ ½±²•·•¬»²¬ ¬»³ó °»®¿¬«®» ¬¸®±«¹¸±«¬ ¬¸» §»¿® ¿²¼ •± »´·³·²¿¬»¼ ±² °±••·¾´» •±«®½» ±º ª¿®·¿¬·±² ©¸»² ³»®¹·²¹ ¼¿¬¿ ±¾¬¿·²»¼ ©»»µ• ±® ³±²¬¸• ¿°¿®¬ò ײ »¿®´§ îðððô ¿ ðòë³ ºñèòï 笽¸»§óݸ®»¬·»² ¬»´»•½±°» ©¿• ·²ó •¬¿´´»¼ ·² ¬¸» •¿³» ¾«·´¼·²¹ ¼»•·¹²»¼ º±® ¬¸» îë½³ ÍÝÌÿ ̸»®» • ²±¬ ³«½¸ ®±±³ ¬± ³±ª» ¿¾±«¬ ¬¸»•» ¼¿§•ÿ ß °±°«´¿® º±½¿´ ®»¼«½»®ô ©·¬¸ ¬¸» ±°¬·½• ®»³±«²¬»¼ ·² ¿ ½«•¬±³ ½»´´ ¬± ¹»¬ ¬¸» ¼»•·¹²»¼ •»°¿®¿¬·±² ¾»¬©»»² ±°¬·½• ¿²¼ ÝÝÜ ½¸·°ô ©¿• «•»¼ ¬± ®»¼«½» ¬¸» •§•¬»³ ¬± ºñìòêò ̸» ®»•«´¬·²¹ º·»´¼ ©¿• ¿¾±«¬ ïç¨ïí ¿®½³·²«¬»• ©¸»² «•·²¹ ¬¸» ÍÌóèò ر©»ª»®ô ·¬ ©¿• ¿´•± •¬®±²¹´§ ª·¹²»¬¬»¼ ¿²¼ •± º´¿¬óº·»´¼• ¾»½¿³» ¿² ¿¾•±´«¬» ³«•¬ º±® ½®·¬·½¿´ ©±®µò ̸»®» ©¿•ô ¿• ³·¹¸¬ ¾» »¨°»½¬»¼ô ¿ º¿·® ¿³±«²¬ ±º ·³¿¹» ¼·•¬±®¬·±² ¬±©¿®¼• ¬¸» »¼¹»•ò ̸»®»º±®»ô ®»º»®»²½» •¬¿®• ¿²¼ ¬¸» ¬¿®¹»¬ ©»®» µ»°¬ ¿• ²»¿® ¬¸» ½»²¬»® ±º ¬¸» ·³¿¹» ¿• °±••·¾´»ò ײ »¿®´§ îððïô ¿ Ú·²¹»® Ô¿µ»• ײ•¬®«³»²¬¿¬·±² ÜÓóïðîì øïðîì¨ïðîì ñ î쫳 Í×Ì» ½¸·° ½¿³»®¿÷ ®»°´¿½»¼ ¬¸» ÍÌóèò ̸·• ¿´´±©»¼ ®»³±ª·²¹ ¬¸» º±½¿´ ®»¼«½»® ¿²¼ ¿½¬«ó ¿´´§ ·²½®»¿•·²¹ ¬¸» •·¦» ±º ¬¸» º·»´¼ ¬± ¿¾±«¬ îð¨îð ¿®½³·²«¬»•ò ̸» ´¿®¹» ½¸·° ¿²¼ ´¿½µ ±º ¬¸» ®»¼«½»® °®±¼«½»• ³«½¸ ¸·¹¸»® ¯«¿´·¬§ ·³¿¹»• ©·¬¸ ²± ª·¹²»¬¬·²¹ ¿²¼ •¸¿®° º±½«• ¿´´ ¬¸» ©¿§ ¬± ¬¸» »¼¹»• ±º ¬¸» º·»´¼ò ß´•±ô ¬¸» ½±±´·²¹ ½¿°¿¾·´·¬·»• ±º ¬¸» ÚÔ× ½¿³»®¿ ¿®» ³«½¸ ¾»¬¬»® ¿²¼ •± ¬¸» ½¿³»®¿ ·• ®«² ¿¬ íð Ýò ̸» ¬»´»•½±°» ¿²¼ ½¿³»®¿ ¿®» ½±²¬®±´´»¼ ©·¬¸ ¾¿®» ¾±²»• л²¬·«³ ××× êíí ®«²²·²¹ É·²¼±©• ÓÛò ß ´»••»® ³¿½¸·²» ©±«´¼ ¿´•± •«ºº·½»ò ̸» ³¿·² ®»¿•±² º±® ¬¸» º¿•¬»® ³¿½¸·²» ·• ¬± ¿½½±³³±¼¿¬» ²»© ½«•¬±³ •±º¬©¿®» ¬¸¿¬ ¿«¬±³¿¬·½¿´´§ •§²½¸®±²·¦»• ¬¸» •½±°» • °±•·¬·±²·²¹ ¾§ ³¿¬½¸ó ·²¹ ¿² ·³¿¹» ¬± ¿² ·²¬»®²¿´ ½¸¿®¬ ½»²¬»®»¼ ±² ¬¸» ®»°±®¬»¼ °±•·¬·±² ±º ¬¸» •½±°»ò ̸» ½±³°«¬»® ·• ´±½¿¬»¼ ·² ³§ ¸±³»ô ¿¾±«¬ íð ³»¬»®• º®±³ ¬¸» ±¾•»®ª¿¬±®§ò Ý¿¾´·²¹ ¿²¼ °±©»® ¿®» ®«² ¬¸®±«¹¸ ¿² è½³ ÐÊÝ °·°» ¾«®·»¼ ¶«•¬ ¿¬ ¹®±«²¼ ´»ª»´ò ̸»®» ¿°°»¿®• ¬± ¾» ²± ·²¬»®º»®»²½» °®±¾´»³• ¼«» ¬± ®«²²·²¹ ¿´´ ¬¸» ½¿¾´»• ¬±¹»¬¸»® ±® ¿ •·¹²·º·½¿²¬ ´±•• ±º •·¹²¿´ •¬®»²¹¬¸ ¼«» ¬± ¬¸» ´»²¹¬¸§ ®«²ò ײ º¿½¬ô ¬¸» ÚÔ× ½¿³»®¿ «•»• •¬¿²¼¿®¼ ÝßÌóë ©·®·²¹ ¿²¼ ¸¿• ¾»»² ¬»•¬»¼ ±«¬ ¬± ¿¾±«¬ ïëð ³»¬»®•ò Û¨°±•«®»• ̸» º±´´±©·²¹ ¬¿¾´» øØ»²¼»² ïççç÷ •¸±©• ¬¸» ´·³·¬·²¹ ³¿¹²·¬«¼» º±® ¿ ¹·ª»² •½±°» ¿²¼ ¿ ¬©± ó³·²«¬» »¨°±•«®»ô ¿•ó •«³·²¹ ¿² ¿ª»®¿¹» ÝÝÜ ½¿³»®¿ ¿²¼ ¹±±¼ •µ§ ½±²¼·¬·±²•æ Ô·³·¬·²¹ ß°»®¬«®» Ó¿¹ò îð ½³ ïíòë ìð ½³ ïëòð ï ³ ïéòð î ³ ïèòë ̸» ®»•¬®·½¬·±² ±º ¬©± ³·²«¬»• ·• •»¬ ¿••«³·²¹ ¬¸» ¿ª»®¿¹» ³±¬·±² ±º ³¿·² ¾»´¬ ¿•¬»®±·¼• ¿²¼ ¿ª±·¼• ¬®¿·´·²¹ ±² ¬¸» ·³¿¹»ò Ú±® º¿•¬»® ±¾¶»½¬•ô •¸±®¬»® ¬·³»• ¿®» ®»¯«·®»¼ ©¸·´» ³±®» ¼·•¬¿²¬ ±¾¶»½¬• ¿´´±© ´±²¹»® »¨°±•«®»•ò Ë•·²¹ ¬¸·• ¬¿¾´» ¿• ¿ ¹«·¼»ô »¨°±•«®»• ©·¬¸ ¬¸» ðòîë³ ÍÝÌ ©»®» çð• ±® ïîð•ô ¼»°»²¼·²¹ ±² ¬¸» ¾®·¹¸¬²»•• ±º ¬¸» ¬¿®¹»¬ ¿•¬»®±·¼ò Ú±® ¬¸» ðòë³ ÎñÝô ©¸»² ©±®µ·²¹ ¿•¬»®±·¼• ïë³ ±® ¾®·¹¸¬»®ô »¨°±•«®»• ±º ¿¾±«¬ êð óçð• ¿®» «•»¼ò ɸ·´» ¿² ÍÒÎ ±º ïðð øðòðï³÷ °®»½·•·±² ·• ¬± ¾» ¼»•·®»¼ô ¹±±¼ ®»•«´¬• ¿• ¼»º·²»¼ ¾§ ¬¸» ¿³±«²¬ ±º ²±·•» ·² ¬¸» °´±¬ó ¬»¼ ¼¿¬¿ ½¿² ¾» ±¾¬¿·²»¼ ©¸»² ¬¸» ÍÒÎ ·• ¿• ´±© ¿• ìðò Ѳ ¬¸» ±¬¸»® ¸¿²¼ô º±® ¬¸±•» ¿•¬»®±·¼• ©¸»®» ¬¸» ¬±¬¿´ ¿ ³ó °´·¬«¼» ·• «²¼»® ðòï³ô ©±®µ·²¹ ¿¬ ¬¸·• ´±©»® ´·³·¬ ±º¬»² °®±¼«½»• ¬±± ¹®»¿¬ ¿ ²±·•» ¬± º·²¼ ¿ °»®·±¼ò ß• ½·®½«³•¬¿²½»• ©±«´¼ ¸¿ª» ·¬ô ´±© ¿³°´·¬«¼» ´±²¹»® °»®·±¼ ¿•¬»®±·¼• ¿®» º¿® ³±®» ½±³³±²ò Ú±® ¬¸» ³±•¬ °¿®¬ ±²´§ ®¿© ·³¿¹»• ¿®» ¬¿µ»²ô ·ò»òô ¬¸±•» ©·¬¸±«¬ ¿ ¼¿®µ º®¿³» ±® º´¿¬óº·»´¼ ³»®¹»¼ ¿¬ ¬¸» ¬·³» ±º ¬¸» »¨°±•«®»ò Ó¿•¬»® ¼¿®µ• ¿²¼ º´¿¬• ¿®» ³»®¹»¼ °®·±® ¬± ³»¿•«®·²¹ ¬¸» ·³¿¹»• º±® °¸±¬±³»¬®§ò ̸·• ¿´´±©• ¬·¹¸¬»® ½±²¬®±´ ±² ¬¸»•» ¬©± ½±³°»²•¿¬·²¹ º®¿³»• ¿²¼ •± ·³°®±ª»¼ ´±²¹ó¬»®³ ¿½½«®¿½§ò ͱº¬©¿®» Ý«•¬±³ •±º¬©¿®» ©®·¬¬»² ¾§ ¬¸» ¿«¬¸±® ·• «•»¼ º±® ·³¿¹» ¿½¯«·•·¬·±²ô ¬»´»•½±°» °±•·¬·±²·²¹ô ¿²¼ °¸±¬±³»¬®·½ ³»¿•ó «®»³»²¬•ò ÓÐÑ Ý±²²»½¬·±²• ·• «•»¼ ¬± ½±²¬®±´ ¬¸» •½±°» ¿²¼ ½¿³»®¿ò ̸·• •±º¬©¿®» ¿´´±©• «²¿¬¬»²¼»¼ •½®·°¬»¼ ±°»®¿¬·±²•ô ·²½´«¼·²¹ ©±®µ·²¹ ³±®» ¬¸¿² ±²» ¬¿®¹»¬ ¿ ²·¹¸¬ò ÓÐÑ Ý¿²±°«• ·• «•»¼ ¬± ³»¿•«®» ¬¸» ·³¿¹»• ¿²¼ ®»ó ¼«½» ¬¸» ¼¿¬¿ º±® ¿•¬®±³»¬®§ ±® «•» ¬¸» ¬·³»ñ³¿¹²·¬«¼» °¿·®• º®±³ ±²» ±® ³±®» ²·¹¸¬• ¬± º·²¼ ¬¸» °»®·±¼ ¿²¼ ¿³°´·¬«¼» ±º ¿² ¿•¬»®±·¼ ´·¹¸¬½«®ª»ò Ý¿²±°«• «•»• ¿°»®¬«®» °¸±¬±³»¬®§ ©·¬¸ ¿ •¯«¿®» ¿²²«´«• ¿²¼ ³»¿•«®·²¹ ¿®»¿ò ̸·• ¹®»¿¬´§ •·³°´·º·»• ³»¿•«®»ó ³»²¬• •·²½» ¬¸»®» ·• ²± ²»»¼ ¬± ¼»¿´ ©·¬¸ °·¨»´• •¬®¿¼¼´·²¹ ¬¸» ¾±«²¼·²¹ ´·²»•ò ß µó•·¹³¿ ½´·°°·²¹ ¿´¹±®·¬¸³ ·• «•»¼ ¬± º·²¼ ¬¸» ¾¿½µ¹®±«²¼ ´»ª»´ ©·¬¸·² ¬¸» ¿²²«´«•ô ©¸·½¸ ·• ¬¸»² •«¾¬®¿½¬»¼ º®±³ ª¿´«»• ©·¬¸·² ¬¸» ³»¿•«®·²¹ ¿® »¿ò ̸» •·¹²¿´ó¬±ó²±·•» ®¿¬·± ·• ½±³°«¬»¼ ¾¿•»¼ ±² ¿ º±®³«´¿ º®±³ α³¿²·•¸·² øîððð÷ô ©¸·½¸ ·²½´«¼»• «•·²¹ ¬¸» »ñßÜË ø»´» ½ó ¬®±²• °»® ß²¿´±¹óÜ·¹·¬¿´ ˲·¬÷ º±® ¬¸» ¹·ª»² ½¿³»®¿ ¿²¼ »¨°±•«®» ¬·³»ò ̸» ¼»®·ª»¼ ª¿´«»• ½±³°¿®» ª»®§ º¿ª±®¿¾´§ ¬± ¬¸±•» ±¾¬¿·²»¼ ©·¬¸ ³«½¸ ³±®» •±°¸·•¬·½¿¬»¼ °¿½µ¿¹»•ò Þ±¬¸ •±º¬©¿®» °®±¹®¿³• ¿®» ½±³³»®½·¿´´§ ¿ª¿·´¿¾´» ¿²¼ ¼»•½®·¾»¼ ±² ¬¸» Ó·²±® д¿²»¬ Ѿ•»®ª»® ©»¾ •·¬» ¿¬ ¸¬¬°æññ©©©òÓ·²±®Ð´¿²»¬Ñ¾•»®ª»®ò½±³ Ù»²»®¿´ Ю±¹®¿³ Ü»•½®·°¬·±² ɸ·½¸ ¿•¬»®±·¼ ¬± ©±®µ ·• ¼»¬»®³·²»¼ ¾§ ¿ °®±½»•• ±º »´·³·²¿¬·±²ò Í»´»½¬·±² «•«¿´´§ •¬¿®¬• ©·¬¸ ²«³¾»®»¼ ¿•¬»®±·¼• ²»¿® ±°°±•·¬·±² ¬¸¿¬ ¿®» ©·¬¸·² ®¿²¹» ±º ¬¸» »¯«·°³»²¬ô «•«¿´´§ ïëòî ±® ¾®·¹¸¬»®ô ¿²¼ ¿®» º¿ª±®¿¾´§ °´¿½»¼ º±® ´»²¹¬¸§ ±ª»®²·¹¸¬ ®«²•ò ̸·• ·²·¬·¿´ ´·•¬ ·• ®»¼«½»¼ ¾§ «•·²¹ ß´¿² Ø¿®®·• ´·•¬ øØ¿®®·• îððï÷ ¿²¼ »´·³·²¿¬·²¹ ¿•¬»®±·¼• º±® ©¸·½¸ ¬¸»®» ¿®» ©»´´óµ²±©² ´·¹¸¬½«®ª»•ò ѽ½¿•·±²¿´´§ô ¿¬¬»²¬·±² ·• ¹·ª»² ¬± ¿² «²«•«¿´ ¿•¬»®±·¼ •«½¸ ¿• ¿² ÒÛÑô ±²» ¾»·²¹ ¬¿®¹»¬»¼ º±® ®¿¼¿® ±¾•»®ª¿¬·±²•ô ±® ±²» ·²ª±´ª»¼ ·² ¿² ±½½«´¬¿¬·±² »ª»²¬ò Ѳ½» ¿² ¿•¬»®±·¼ ·• •»´»½¬»¼ ¾«¬ ¾»º±®» ±¾•»®ª¿¬·±²• ¾»¹·²ô ·³¿¹»• ¿®» ¬¿µ»² ±º ¿ ²»¿®¾§ º·»´¼ ©·¬¸ •¬¿®• ±º ³»¼·«³ ¬± ¸·¹¸ ¿½½«®¿½§ ³¿¹²·¬«¼»•ò ̸» ÔÑÒÛÑÍ ½¿¬¿´±¹ô °®±¼«½»¼ ¾§ Þ®·¿² ͵·ºº ¿¬ Ô±©»´´ Ѿ•»®ª¿¬±®§ô Ú´¿¹•¬¿ººô ßÆô ·• ±º¬»² «•»¼ º±® ¬¸·• °«®°±•»ò Þ»º±®» ¬¸» •¬¿®¬ ±º ¬¸» ®«²ô ¿¬ ¬¸» »²¼ô ¿²¼ ¿¬ ´»¿•¬ ±²½» ·² ¾»¬©»»²ô ¬¸·• º·»´¼ ·• ·³¿¹»¼ ¿¬ ¬¸» •¿³» ¬»³°»®¿¬«®» ¿²¼ »¨°±•«®» ¿• ¬¸» ·³¿¹»• º±® ¬¸» ´·¹¸¬½«®ª» ©±®µò ̸» °¸±¬±³»¬®§ °®±¹®¿³ ³»¿•«®»• ¬¸»•» ·³¿¹»• ¬± ¼»¬»®³·²» ¬¸» ³¿¹²·¬«¼» ª•ò ·²¬»²•·¬§ ®»´¿¬·±²•¸·° º±® ¬¸» ®«²ô ·ò»òô ·¬ ½¿´·¾®¿¬»• ¬¸» °¸±¬±³»¬®§ò Ü»°»²¼·²¹ ±² ¬¸» ¬§°» ±º ¿•¬»®±·¼ ¿²¼ ¬¸» ´·µ»´·¸±±¼ ±º ·¬ ¾»·²¹ ¿ º¿•¬ ®±¬¿¬±®ô ·³¿¹»• ¿®» ¬¿µ»² ¿¬ ·²¬»®ª¿´• ®¿²¹·²¹ º®±³ ï ¬± í ³·²«¬»•ô ©·¬¸ î ³·²«¬»• ¾»·²¹ °®»º»®®»¼ ¿• ·¬ °®±ª·¼»• ¿ •³±±¬¸»® •»¬ ±º ¼¿¬¿ ¿²¼ ¿´´±©• º»¿¬«®»• ©·¬¸·² ¬¸» ½«®ª» ¬± ¾» ³±®» ®»¿¼·´§ ·¼»²¬·º·»¼ò ׳¿¹»• ¿®» ¬¿µ»² º±® ¿• ´±²¹ ¿• ½±²¼·¬·±²• ¿´´±©ô »ò¹òô ¾»¹·²²·²¹ ±º ¬©·´·¹¸¬ ±® ¬¸» ¿•¬»®±·¼ ¹»¬• ¾»´±© íð ¿´¬·¬«¼»ò É·¬¸ ¬¸» •±º¬©¿®» ¬¿µ·²¹ ½¿®» ±º »ª»®§¬¸·²¹ô ±²´§ ¿ º»© ½¸»½µ• ¿®» ®»¯«·®»¼ ¬¸®±«¹¸±«¬ ¬¸» ²·¹¸¬ ¬± ³¿µ» •«®» ¬¸» ¿•¬»®±·¼ ·• ²±¬ ³±ª·²¹ ±«¬ ±º ¬¸» º·»´¼ ¿²¼ ¬¸¿¬ ¬¸» º±½«• ·• •¬·´´ ¿½½»°¬¿¾´»ò ̸» ÓÐÑ Ý±²²»½¬·±²• •±º¬©¿®» ¼±»• ¸¿ª» ¿² ¿«¬±º±½«• ®±«¬·²» ¬¸¿¬ ½¿² ¾» °¿®¬ ±º ¬¸» •½®·°¬ ¾«¬ô º±® ²±©ô ¬¸» ¬»´»•½±°» ¼±»• ²±¬ ¸¿ª» ¬¸» ²»½»••¿®§ ¸¿®¼©¿®»ò Ü¿¬¿ λ¼«½¬·±² ß• ³»²¬·±²»¼ ¿¾±ª»ô ÓÐÑ Ý¿²±°«• ·• «•»¼ º±® ¼¿¬¿ ®»¼«½¬·±²ò ̸·• °®±¹®¿³ ·• «•»¼ ¬± ³»¿•«®» ¬¸» ÔÑÒÛÑÍ ®»º»®»²½» º·»´¼ ¿²¼ ¬¸» ·²¼·ª·¼«¿´ ·³ó ¿¹»•ò Ú·®•¬ô ±²» ±º ¬¸» ®»º»®»²½» º·»´¼• ·• ³»¿•«®»¼ ¬± º·²¼ ¿ ´»¿•¬ •¯«¿®»• •±´«¬·±² ¾¿•»¼ ±² ¬¸» ½¿¬¿ó ´±¹ ³¿¹²·¬«¼» ¿²¼ ¬¸» ¬±¬¿´ ·²¬»²•·¬§ º±® »¿½¸ •¬¿®ò ̸·• ¸¿• °®±ª»¼ •«ºº·½·»²¬ º±® ¾¿•·½ ¼·ºº»®»²¬·¿´ °¸±ó ¬±³»¬®§ô »ª»² ©¸»² ©±®µ·²¹ ¬¸» ¿•¬»®±·¼ ·² ¼·ºº»®»²¬ º·»´¼• ±ª»® ¿ °»®·±¼ ±º ¬·³»ò ر©»ª»®ô º±® ½±´´¿¾±®¿ó ¬·ª» ©±®µ ±® ¼»¬»®³·²·²¹ ¬¸» Ø ¿²¼ Ù °¸¿•» ª¿´«»•ô ¿ •»°¿®¿¬» °®±¹®¿³ô ÐØÑÌÑÎÛÜô ½¿² ¾» «•»¼ ¬± ¼»¬»®³·²» ¬¸» ²·¹¸¬´§ ¬®¿²•º±®³¿¬·±² ª¿´«»• ¿²¼ ®»¼«½» ¬¸» ¼¿¬¿ ¬± ¿ •¬¿²¼¿®¼ •§•¬»³ò Ú±® »¿½¸ ¿•¬»®±·¼ ·³¿¹»ô ¬¸» º±´´±©·²¹ ·²º±®³¿¬·±² ·• •¬±®»¼ ·² ¿ ¼¿¬¿¾¿•»æ i ËÌ Ü¿¬»ñÌ·³» ±º ³·¼ó»¨°±•«®» i ̸» ¼»®·ª»¼ ³¿¹²·¬«¼» ±º ¬¸» ¿•¬»®±·¼ ¿²¼ ½±³°¿®·•±² •¬¿®• ¿• ¼»¬»®³·²»¼ ¾§ ¿ ´»¿•¬ •¯«¿®»• •±´«¬·±² « •ó ·²¹ ½¿¬¿´±¹ ³¿¹²·¬«¼»• ¿²¼ ¬¸» ³»¿•«®»¼ ¬±¬¿´ ·²¬»²•·¬§ ±º ¬¸» •¬¿®ò i ̸» ®¿© ·²•¬®«³»²¬¿´ ³¿¹²·¬«¼» ±º ¬¸» ¿•¬»®±·¼ º±® «•» ©¸»² ®»¼«½·²¹ ³»¿•«®»³»²¬• ¬± ¿ •¬¿²¼¿®¼ •§•¬»³ò i ̸» ¿ª»®¿¹» ³¿¹²·¬«¼» ±º ¬¸» ½±³°¿®·•±² •¬¿®• i ̸» ݱ³°¿®·•±² ó ß•¬»®±·¼
Load more

Recommended publications
  • Annualreport2005 Web.Pdf
    Vision Statement The Space Science Institute is a thriving center of talented, entrepreneurial scientists, educators, and other professionals who make outstanding contributions to humankind’s understanding and appreciation of planet Earth, the Solar System, the galaxy, and beyond. 2 | Space Science Institute | Annual Report 2005 From Our Director Excite. Explore. Discover. These words aptly describe what we do in the research realm as well as in education. In fact, they defi ne the essence of our mission. Our mission is facilitated by a unique blend of on- and off-site researchers coupled with an extensive portfolio of education and public outreach (EPO) projects. This past year has seen SSI grow from $4.1M to over $4.3M in grants, an increase of nearly 6%. We now have over fi fty full and part-time staff. SSI’s support comes mostly from NASA and the National Sci- ence Foundation. Our Board of Directors now numbers eight. Their guidance and vision—along with that of senior management—have created an environment that continues to draw world-class scientists to the Institute and allows us to develop educa- tion and outreach programs that benefi t millions of people worldwide. SSI has a robust scientifi c research program that includes robotic missions such as the Mars Exploration Rovers, fl ight missions such as Cassini and the Spitzer Space Telescope, Hubble Space Telescope (HST), and ground-based programs. Dr. Tom McCord joined the Institute in 2005 as a Senior Research Scientist. He directs the Bear Fight Center, a 3,000 square-foot research and meeting facility in Washington state.
    [Show full text]
  • The Composition of M-Type Asteroids II: Synthesis of Spectroscopic and Radar Observations ⇑ J.R
    Icarus 238 (2014) 37–50 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus The composition of M-type asteroids II: Synthesis of spectroscopic and radar observations ⇑ J.R. Neeley a,b,1, , B.E. Clark a,1, M.E. Ockert-Bell a,1, M.K. Shepard c,2, J. Conklin d, E.A. Cloutis e, S. Fornasier f, S.J. Bus g a Department of Physics, Ithaca College, Ithaca, NY 14850, United States b Department of Physics, Iowa State University, Ames, IA 50011, United States c Department of Geography and Geosciences, Bloomsburg University, Bloomsburg, PA 17815, United States d Department of Mathematics, Ithaca College, Ithaca, NY 14850, United States e Department of Geography, University of Winnipeg, Winnipeg, MB R3B 2E9, Canada f LESIA, Observatoire de Paris, 5 Place Jules Janssen, F-92195 Meudon Principal Cedex, France g Institute for Astronomy, 2680 Woodlawn Dr., Honolulu, HI 96822, United States article info abstract Article history: This work updates and expands on results of our long-term radar-driven observational campaign of Received 7 February 2012 main-belt asteroids (MBAs) focused on Bus–DeMeo Xc- and Xk-type objects (Tholen X and M class Revised 7 May 2014 asteroids) using the Arecibo radar and NASA Infrared Telescope Facilities (Ockert-Bell, M.E., Clark, B.E., Accepted 9 May 2014 Shepard, M.K., Rivkin, A.S., Binzel, R.P., Thomas, C.A., DeMeo, F.E., Bus, S.J., Shah, S. [2008]. Icarus 195, Available online 16 May 2014 206–219; Ockert-Bell, M.E., Clark, B.E., Shepard, M.K., Issacs, R.A., Cloutis, E.A., Fornasier, S., Bus, S.J.
    [Show full text]
  • The Minor Planet Bulletin
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 3, A.D. 2009 JULY-SEPTEMBER 77. PHOTOMETRIC MEASUREMENTS OF 343 OSTARA Our data can be obtained from http://www.uwec.edu/physics/ AND OTHER ASTEROIDS AT HOBBS OBSERVATORY asteroid/. Lyle Ford, George Stecher, Kayla Lorenzen, and Cole Cook Acknowledgements Department of Physics and Astronomy University of Wisconsin-Eau Claire We thank the Theodore Dunham Fund for Astrophysics, the Eau Claire, WI 54702-4004 National Science Foundation (award number 0519006), the [email protected] University of Wisconsin-Eau Claire Office of Research and Sponsored Programs, and the University of Wisconsin-Eau Claire (Received: 2009 Feb 11) Blugold Fellow and McNair programs for financial support. References We observed 343 Ostara on 2008 October 4 and obtained R and V standard magnitudes. The period was Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids”, found to be significantly greater than the previously Icarus 72, 135-208. reported value of 6.42 hours. Measurements of 2660 Wasserman and (17010) 1999 CQ72 made on 2008 Stecher, G.J., Ford, L.A., and Elbert, J.D. (1999). “Equipping a March 25 are also reported. 0.6 Meter Alt-Azimuth Telescope for Photometry”, IAPPP Comm, 76, 68-74. We made R band and V band photometric measurements of 343 Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry Ostara on 2008 October 4 using the 0.6 m “Air Force” Telescope and Analysis. Springer, New York, NY. located at Hobbs Observatory (MPC code 750) near Fall Creek, Wisconsin.
    [Show full text]
  • The Minor Planet Bulletin and How the Situation Has Gone from One Mt Tarana Observatory of Trying to Fill Pages to One of Fitting Everything In
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 33, NUMBER 2, A.D. 2006 APRIL-JUNE 29. PHOTOMETRY OF ASTEROIDS 133 CYRENE, adjusted up or down to line up with the V-band data). The near- 454 MATHESIS, 477 ITALIA, AND 2264 SABRINA perfect overlay of V- and R-band data show no evidence of color change as the asteroid rotates. This result replicates the lightcurve Robert K. Buchheim period reported by Harris et al. (1984), and matches the period and Altimira Observatory lightcurve shape reported by Behrend (2005) at his website. 18 Altimira, Coto de Caza, CA 92679 USA [email protected] (Received: 4 November Revised: 21 November) Photometric studies of asteroids 133 Cyrene, 454 Mathesis, 477 Italia and 2264 Sabrina are reported. The lightcurve period for Cyrene of 12.707±0.015 h (with amplitude 0.22 mag) confirms prior studies. The lightcurve period of 8.37784±0.00003 h (amplitude 0.32 mag) for Mathesis differs from previous studies. For Italia, color indices (B-V)=0.87±0.07, (V-R)=0.48±0.05, and phase curve parameters H=10.4, G=0.15 have been determined. For Sabrina, this study provides the first reported lightcurve period 43.41±0.02 h, with 0.30 mag amplitude. Altimira Observatory, located in southern California, is equipped with a 0.28-m Schmidt-Cassegrain telescope (Celestron NexStar- 454 Mathesis. DiMartino et al. (1994) reported a rotation period of 11 operating at F/6.3), and CCD imager (ST-8XE NABG, with 7.075 h with amplitude 0.28 mag for this asteroid, based on two Johnson-Cousins filters).
    [Show full text]
  • Für Astronomie Nr
    für Astronomie Nr. 28 Zeitschrift der Vereinigung der Sternfreunde e.V. / VdS DAS WELTALL Orionnebel DU LEBST DARIN – ENTDECKE ES! Computerastronomie Internationales Jahr der Astronomie INTERNATIONALES ISSN 1615 - 0880 www.vds-astro.de I/ 2009 ASTRONOMIEJAHR [email protected] • www.astro-shop.com Tel.: 040/5114348 • Fax: 040/5114594 Eiffestr. 426 • 20537 Hamburg Astroart 4.0 The Night Sky Observer´s Guide Photoshop Astronomy Die aktuellste Version Dieses hilfreiche Werk Der Autor arbeitet seit fast 10 Jahren mit Photo- des bekannten Bildbe- dient der erfolg- shop, um seine Astrofotos zu bearbeiten. Die arbeitungspro- reichen Vorbereitung dabei gemachten Erfahrungen hat er in diesem grammes gibt es jetzt einer abwechslungs- speziell auf die Bedürfnisse des Amateurastro- mit interessanten reichen Deep-Sky- nomen zugeschnitte- neuen Funktionen. Nacht. Sortiert nach nen Buch gesammelt. Moderne Dateifor- Sternbildern des Die behandelten The- men sind unter ande- mate wie DSLR-RAW Sommer- und Win- rem: die technische werden unterstützt, terhimmels nden Ausstattung, Farbma- Bilder können sich detaillierte NEU nagement, Histo- durch automa- Beschreibungen Südhimmel gramme, Maskie- 3. Band tische Sternfelderken- zu hunderten rungstechniken, nung direkt überlagert werden, was die Bild- Galaxien, Nebeln, Oenen Stern- und Addition mehrerer feldrotation vernachlässigbar macht. Auch die Kugelhaufen. Der Teleskopanblick jedes Bilder, Korrektur von Bearbeitung von Farbbildern wurde erweitert. Objekts ist beschrieben und mit einem Hin- Vignettierungen, Besonderes Augenmerk liegt auf der Erken- weis bezüglich der verwendeten Optik verse- Farbhalos, Deformationen oder nung und Behandlung von Pixelfehlern der hen. 2 Bände mit insgesamt 446 Fotos, 827 überbelichteten Sternen, LRGB und vieles Aufnahme-Chips. Zeichnungen, 143 Tabellen und 431 Sternkar- mehr. Auf der beigefügten DVD benden sich 90 alle im Buch besprochenen und verwendeten Update ten.
    [Show full text]
  • Multi-Messenger Observations of a Binary Neutron Star Merger
    DRAFT VERSION OCTOBER 6, 2017 Typeset using LATEX twocolumn style in AASTeX61 MULTI-MESSENGER OBSERVATIONS OF A BINARY NEUTRON STAR MERGER LIGO SCIENTIFIC COLLABORATION,VIRGO COLLABORATION AND PARTNER ASTRONOMY GROUPS (Dated: October 6, 2017) ABSTRACT On August 17, 2017 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB170817A) with a time-delay of 1.7swith respect to the merger ⇠ time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance +8 of 40 8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range− 0.86 to 2.26 M . An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT2017gfo) in NGC 4993 (at 40 Mpc) less ⇠ than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1-m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over 10 days. Following early non-detections, X-ray and radio emission were discovered at the ⇠ transient’s position 9 and 16 days, respectively, after the merger.
    [Show full text]
  • An Anisotropic Distribution of Spin Vectors in Asteroid Families
    Astronomy & Astrophysics manuscript no. families c ESO 2018 August 25, 2018 An anisotropic distribution of spin vectors in asteroid families J. Hanuš1∗, M. Brož1, J. Durechˇ 1, B. D. Warner2, J. Brinsfield3, R. Durkee4, D. Higgins5,R.A.Koff6, J. Oey7, F. Pilcher8, R. Stephens9, L. P. Strabla10, Q. Ulisse10, and R. Girelli10 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holešovickáchˇ 2, 18000 Prague, Czech Republic ∗e-mail: [email protected] 2 Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908, USA 3 Via Capote Observatory, Thousand Oaks, CA 91320, USA 4 Shed of Science Observatory, 5213 Washburn Ave. S, Minneapolis, MN 55410, USA 5 Hunters Hill Observatory, 7 Mawalan Street, Ngunnawal ACT 2913, Australia 6 980 Antelope Drive West, Bennett, CO 80102, USA 7 Kingsgrove, NSW, Australia 8 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA 9 Center for Solar System Studies, 9302 Pittsburgh Ave, Suite 105, Rancho Cucamonga, CA 91730, USA 10 Observatory of Bassano Bresciano, via San Michele 4, Bassano Bresciano (BS), Italy Received x-x-2013 / Accepted x-x-2013 ABSTRACT Context. Current amount of ∼500 asteroid models derived from the disk-integrated photometry by the lightcurve inversion method allows us to study not only the spin-vector properties of the whole population of MBAs, but also of several individual collisional families. Aims. We create a data set of 152 asteroids that were identified by the HCM method as members of ten collisional families, among them are 31 newly derived unique models and 24 new models with well-constrained pole-ecliptic latitudes of the spin axes.
    [Show full text]
  • Asteroid Regolith Weathering: a Large-Scale Observational Investigation
    University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 5-2019 Asteroid Regolith Weathering: A Large-Scale Observational Investigation Eric Michael MacLennan University of Tennessee, [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Recommended Citation MacLennan, Eric Michael, "Asteroid Regolith Weathering: A Large-Scale Observational Investigation. " PhD diss., University of Tennessee, 2019. https://trace.tennessee.edu/utk_graddiss/5467 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Eric Michael MacLennan entitled "Asteroid Regolith Weathering: A Large-Scale Observational Investigation." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Geology. Joshua P. Emery, Major Professor We have read this dissertation and recommend its acceptance: Jeffrey E. Moersch, Harry Y. McSween Jr., Liem T. Tran Accepted for the Council: Dixie L. Thompson Vice Provost and Dean of the Graduate School (Original signatures are on file with official studentecor r ds.) Asteroid Regolith Weathering: A Large-Scale Observational Investigation A Dissertation Presented for the Doctor of Philosophy Degree The University of Tennessee, Knoxville Eric Michael MacLennan May 2019 © by Eric Michael MacLennan, 2019 All Rights Reserved.
    [Show full text]
  • Clasificación Taxonómica De Asteroides
    Clasificación Taxonómica de Asteroides Cercanos a la Tierra por Ana Victoria Ojeda Vera Tesis sometida como requisito parcial para obtener el grado de MAESTRO EN CIENCIAS EN CIENCIA Y TECNOLOGÍA DEL ESPACIO en el Instituto Nacional de Astrofísica, Óptica y Electrónica Agosto 2019 Tonantzintla, Puebla Bajo la supervisión de: Dr. José Ramón Valdés Parra Investigador Titular INAOE Dr. José Silviano Guichard Romero Investigador Titular INAOE c INAOE 2019 El autor otorga al INAOE el permiso de reproducir y distribuir copias parcial o totalmente de esta tesis. II Dedicatoria A mi familia, con gran cariño. A mis sobrinos Ian y Nahil, y a mi pequeña Lia. III Agradecimientos Gracias a mi familia por su apoyo incondicional. A mi mamá Tere, por enseñarme a ser perseverante y dedicada, y por sus miles de muestras de afecto. A mi hermana Fernanda, por darme el tiempo, consejos y cariño que necesitaba. A mi pareja Odi, por su amor y cariño estos tres años, por su apoyo, paciencia y muchas horas de ayuda en la maestría, pero sobre todo por darme el mejor regalo del mundo, nuestra pequeña Lia. Gracias a mis asesores Dr. José R. Valdés y Dr. José S. Guichard, promotores de esta tesis, por su paciencia, consejos y supervisión, y por enseñarme con sus clases divertidas y motivadoras todo lo que se refiere a este trabajo. A los miembros del comité, Dra. Raquel Díaz, Dr. Raúl Mújica y Dr. Sergio Camacho, por tomarse el tiempo de revisar y evaluar mi trabajo. Estoy muy agradecida con todos por sus críticas constructivas y sugerencias.
    [Show full text]
  • Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1
    Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 1 LESIA, Observatoire de Paris, CNRS, UPMC Univ Paris 06, Univ. Paris Diderot, 5 Place J. Janssen, 92195 Meudon Pricipal Cedex, France 2 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris Cedex 13 3 Department of Physics and Astronomy of the University of Padova, Via Marzolo 8 35131 Padova, Italy Submitted to Icarus: November 2013, accepted on 28 January 2014 e-mail: [email protected]; fax: +33145077144; phone: +33145077746 Manuscript pages: 38; Figures: 13 ; Tables: 5 Running head: Aqueous alteration on primitive asteroids Send correspondence to: Sonia Fornasier LESIA-Observatoire de Paris arXiv:1402.0175v1 [astro-ph.EP] 2 Feb 2014 Batiment 17 5, Place Jules Janssen 92195 Meudon Cedex France e-mail: [email protected] 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 062.S-0173 and 064.S-0205 (PI M. Lazzarin) Preprint submitted to Elsevier September 27, 2018 fax: +33145077144 phone: +33145077746 2 Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 Abstract This work focuses on the study of the aqueous alteration process which acted in the main belt and produced hydrated minerals on the altered asteroids. Hydrated minerals have been found mainly on Mars surface, on main belt primitive asteroids and possibly also on few TNOs. These materials have been produced by hydration of pristine anhydrous silicates during the aqueous alteration process, that, to be active, needed the presence of liquid water under low temperature conditions (below 320 K) to chemically alter the minerals.
    [Show full text]
  • Creation and Application of Routines for Determining Physical Properties of Asteroids and Exoplanets from Low Signal-To-Noise Data Sets
    University of Central Florida STARS Electronic Theses and Dissertations, 2004-2019 2014 Creation and Application of Routines for Determining Physical Properties of Asteroids and Exoplanets from Low Signal-To-Noise Data Sets Nathaniel Lust University of Central Florida Part of the Astrophysics and Astronomy Commons, and the Physics Commons Find similar works at: https://stars.library.ucf.edu/etd University of Central Florida Libraries http://library.ucf.edu This Doctoral Dissertation (Open Access) is brought to you for free and open access by STARS. It has been accepted for inclusion in Electronic Theses and Dissertations, 2004-2019 by an authorized administrator of STARS. For more information, please contact [email protected]. STARS Citation Lust, Nathaniel, "Creation and Application of Routines for Determining Physical Properties of Asteroids and Exoplanets from Low Signal-To-Noise Data Sets" (2014). Electronic Theses and Dissertations, 2004-2019. 4635. https://stars.library.ucf.edu/etd/4635 CREATION AND APPLICATION OF ROUTINES FOR DETERMINING PHYSICAL PROPERTIES OF ASTEROIDS AND EXOPLANETS FROM LOW SIGNAL-TO-NOISE DATA-SETS by NATE B LUST B.S. University of Central Florida, 2007 A dissertation submitted in partial fulfilment of the requirements for the degree of Doctor of Philosophy in Physics in the Department of Physics in the College of Sciences at the University of Central Florida Orlando, Florida Fall Term 2014 Major Professor: Daniel Britt © 2014 Nate B Lust ii ABSTRACT Astronomy is a data heavy field driven by observations of remote sources reflecting or emitting light. These signals are transient in nature, which makes it very important to fully utilize every observation.
    [Show full text]
  • The Minor Planet Bulletin
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 38, NUMBER 2, A.D. 2011 APRIL-JUNE 71. LIGHTCURVES OF 10452 ZUEV, (14657) 1998 YU27, AND (15700) 1987 QD Gary A. Vander Haagen Stonegate Observatory, 825 Stonegate Road Ann Arbor, MI 48103 [email protected] (Received: 28 October) Lightcurve observations and analysis revealed the following periods and amplitudes for three asteroids: 10452 Zuev, 9.724 ± 0.002 h, 0.38 ± 0.03 mag; (14657) 1998 YU27, 15.43 ± 0.03 h, 0.21 ± 0.05 mag; and (15700) 1987 QD, 9.71 ± 0.02 h, 0.16 ± 0.05 mag. Photometric data of three asteroids were collected using a 0.43- meter PlaneWave f/6.8 corrected Dall-Kirkham astrograph, a SBIG ST-10XME camera, and V-filter at Stonegate Observatory. The camera was binned 2x2 with a resulting image scale of 0.95 arc- seconds per pixel. Image exposures were 120 seconds at –15C. Candidates for analysis were selected using the MPO2011 Asteroid Viewing Guide and all photometric data were obtained and analyzed using MPO Canopus (Bdw Publishing, 2010). Published asteroid lightcurve data were reviewed in the Asteroid Lightcurve Database (LCDB; Warner et al., 2009). The magnitudes in the plots (Y-axis) are not sky (catalog) values but differentials from the average sky magnitude of the set of comparisons. The value in the Y-axis label, “alpha”, is the solar phase angle at the time of the first set of observations. All data were corrected to this phase angle using G = 0.15, unless otherwise stated.
    [Show full text]