238 CERARDI REGNERI fOCKENS 



<( far as the ncw dbservations are concemed , my forracr conclusions have been sfrengh« 

 « lened instead of weakened. I do not mean, however, lo assert, Ihat the subjecl ia 

 « yet diverted of Ihe difficullies attendant on it from olher sources. Some of the resulti 

 « ihat I have found , altliough in themselves in no manner inconsistent with parallax, 

 « will , justly pcrhaps Mith many , add to the difflculty of admilting the explanation by 

 « parallax. They will be unwilling lo admit ihat many of the smailer stars are nearer 

 « to U3 ihan many of the brighter. That in a cerlain pari of the beavens of cousidera» 

 « ble extent, many of the stars exhibit a sensible parallax. This however must be ad- 

 « milted, if my discordances result from parallax. If it be admitted, then several of 

 « ihe difRculties that have occurred by comparing my observations and those of Mr. 

 « Pond, will be done away. Biit I shall dcfer a few remarks on this head, tili I 

 « have given an account of my own observations, and of the results thereof. " 



Reduclionem observalionum bis verbis indicat firinkleius: 



« The observed zenith dislances of a given star were reduced to Jant 1 , 1819 , by 

 « Ihe common equations , taking the constant of aberration = 20",23. The mean of 

 « Ihese were taken, The correet mean zenilh distance was supposed equal to this 

 n raean — e, the constant of aberration = 20,23 + x, and the semiparallax r= p, 

 « The equations of condilion resulting from the respective observations thus contained 

 «( three unknown quantities. These equations were reduced to three , by the melhod 

 « oi making the sum of the Squares of the errors a minimum. The Solutions of these 

 « three equations give the values of e , x and p , and thence the valucs of the mean 

 H polar distance , constant of aberration , and semiparallax. " 

 eventum autem hoc modo ; 



« The parallax resulting for a Lyrae does not malerially differ from my first determi- 



« nation. That of ot Aquilae is less than before The parallax of Arclurus is 



« some what less than before, and that of r Cygni considerably less. y Oraoouis, as 

 « before, exhibils iio parallax. The small negative result of y§g of a second may safely 

 « be referred lo the uiiavoidable errors of Observation. The new results agree wilh the 

 (( former , in showing that the Poleslar has no sensible parallax. " 

 conclusionem ita : 



« In considering the results with a view lo the question of parallax , wbether those 

 « that appear to point out parallax have not an origin in some cause unconnected with 

 « parallax: the first remark that offers itself is, that all Ihe results fnsnish a pa'ylive 

 «parallax, if we except those small quantities in three of the slars wliich are (juite 

 V, with in the limils of the unavoidable errors of Observation. Might it not be expecLed 

 « that some of the stars would have furuished negative, as great as the positive quan* 



« li- 



