ally; though notwithstanding this, the surface 

 these regions cannot be in a condition of perfect calm ; for 

 the appearance of small jets, and the irregularity and varia- 

 bility of the chromosphere, show that even in those regions 

 there is a state of continuous eruption, though on a very- 

 small scale. 



Considering the whole body of observations made, it appears 

 that the northern hemisphere is perceptibly more character- 

 ized by great protuberances and gigantic eruptions than the 

 southern, and that in the former large protuberances are on 

 rare occasions seen at distances less than 20° from the pole, 

 a thing which never happens in the southern hemisphere. In 

 the vicinity of the equator, protuberances of great size occur 

 less frequently than in higher latitudes. 



As to the connection of the protuberances with the faculae, 

 It is found that the latter are commonly accompanied by protu- 

 berances of considerable size, though without being confounded 

 with them in the same phenomenon. Thus it would appear to 

 be proved that the faculae are special modifications of the photo- 

 sphere in the neighborhood of powerful eruptions. 



The following results have been deduced from a great num- 

 ber of observations made upon the border of the sun's disk, in 

 the region of the spots :- 



1. In the neighborhood of the spots the chromosphere [straUy 

 rosato) is rather low, quite regular and intensely bright. 



2. Upon the exact locality of a spot, or rather over its nu- 

 cleus, the chromosphere is generally very low and sometimes 

 totally wanting. ^ ^ ^ ^ ^ 



3. At the nucleus, either there are no eruptions or they are 

 confined to jets of gn ' ' 



4. The nuclei of tl 

 sess very feeble 1 



Y; Along the borders of the spots, jets are thrown up of extra- 

 ordmary intensity and violence and of very definite configuration. 



6. The jets adjoining the spots consist not solely of hydro- 

 gen, but also of other substances, as is shown by their respec- 

 tive bright lines in the spectrum. ^ ^ 

 ., '-Among these bright lines which are commonly found a 

 tne base or in the lower portions of the j 



the red, one between C and B, distant from G ^Vo of 

 7" ■'pa^e C—B ; the other is between B and a, distant from a 

 Tso of the space B— a. These lines do not correspond with 

 tboseof any substance yet known. They are also not mfre- 

 quently seen quite bright in the highest parts of the jets. 



8- Now and then the eruptions in the vicinity of the spots 

 ^^e gigantic proportions, and are probably the cause of the 



