Angle from North Point through the East to First Point of Contact.

Longitude West from Greenwich.

70° 71° 72° 73° 74°

75° 76° 77° 78° 79°

80° 81° 82° 83° 84° 85° 86° 87° 88° 89° 90° 91° 92° 93°

Latitude.

30

31
32

о

O
O
O
358 354 351 349
344 343

340

339

336

335

46 311

309

O
O
359 353 350
O
359 355 351 347 345
344
348 346 344 342 341 340
33 352 349 347 316
341 340 339 338 337
34 346 341 342 341
336 335 334 333 332
35 340 339 338 337
334 333
36 336 336 335 334 333 332 331 330
37 333 333 332 331 330 329 328 327
38 330 330 329 328 327 326 325
324
39 327 327 326 325 324 323 322
40 324 324 323 322 321 3:20 319 319 318
41
321 321 321 319
319 318 317 317 316
42 319 318 318 317 317 317 316 316 315 314 313 312
43 317 316 316 315 315 315 314 314 313 313 312 311
44 315 314 314 313 313 313 312 312 311 311 310 309
45 313 312 312 311 311 311 310 310 309 309 30S 307
310 310 309
309 308 308 308 307

о

342

341

340

338

337

336

335

333

332

331

330

330

47 309

308 308 307

307

307 306 306

306

305 305

304

304

303

303 302

302

301

301 300

300

299

299

298

Latitude.

Elements of the Eclipse, by which it may be computed for any Place, with the greatest accuracy.

These tables are adapted to computation by the following modification of Bessel's formulæ, which was suggested by T. Henry Safford, Jr.

the latitude of the place.

λ=its eastern longitude from Greenwich.

log. e 8.9110835

log. (1-2)=9.9971066

sin.ye sin.

hsec. cos.

k=(1—e2) sec. y sin.

a=A―h sin. ( μ+2)

b = B− Ek+Hh cos. (u+2)

c=-C+Fk— Gh cos. (u+2)

m=√(bc)

If the instant for computation were correctly chosen at the time of beginning or end of the eclipse, m would be exactly equal to a. If m is not equal to a, the instant for a new computation, and which will be an approximation to the actual time of beginning, may be found by adding to the preceding time of computation an interval t, which may be obtained in seconds by the formulæ

and if is taken of the same sign with a, it is a sufficiently near approximation to the angle of contact from the north towards the east. The magnitude of the eclipse is found by taking the difference (with regard to the signs) of at the beginning and end of the eclipse, and if this difference is denoted by 24, the magnitude of the eclipse is

The value of o may also be obtained by the formula

The elements of the sun for this table were derived from Bessel's tables, those of the moon from Damoiseau's tables corrected by Airy for Plana's theory, and with the additional corrections given by Hansen's new terms and by Airy's comparison with the Greenwich Observations.

The following is an example under these tables for the computation of the beginning of the eclipse for the Washington Observatory.