RASC OBSERVER’S HANDBOOK 2013

Dwarf anD Minor Planets 245

PLANETARY OCCULTATIONSby DaviD W. Dunham, James stamm, steve Preston, anD Derek breit

IntroductionAs major, dwarf, and minor planets (with their satellites) move across the sky, they occasionally pass directly between an observer and a distant star, producing an occultation. Astronomers have learned much about Solar System bodies by carefully monitoring the changing apparent brightness of stars during the immersion and emersion phases of occultations. If the occulting body does not have an atmosphere, the occultation is virtually instantaneous; if there is an atmosphere, the star disappears and reappears gradually. If a planet has rings or other debris in its environs, the extent and degree of transparency of this material can be precisely mapped. The rings of Uranus, the ring arcs of Neptune, and the atmosphere of Pluto were all discovered by occultation observations. If an occultation is observed at several distributed sites, the size and shape of the occulting body can be determined more accurately than by other Earth-based techniques.

Amateur astronomers can often make important contributions to occultation observing campaigns. This is particularly true for minor planet occultations, for which the paths across the Earth’s surface are often very narrow and uncertain in location (due to uncertainties in both the star’s position and in the ephemeris of the minor planet). By recording the times of the star’s disappearance and reappearance as seen from several sites (i.e. by noting the edges of the minor planet’s shadow as it sweeps across Earth), the object’s profile can be directly determined. Often timings of ade-quate accuracy can be made by visual observers using modest telescopes.

When observing an occultation, it is important to pinpoint the site to within a fraction of a kilometre. Geographic latitude and longitude, as well as the altitude of an observing site, can be determined with a GPS receiver, from a high-quality topo-graphic map, or from some map websites. For observations of maximum value, the immersion and emersion times must be determined as accurately as possible—cer-tainly to better than 0.5 s, and better than 0.2 s for the shortest events (those less than 10 s in duration). Photoelectric equipment with high-speed digital recording systems is well-suited for this work. Attaching a low-light-level video camera to a telescope is a less expensive method for accurate timing. Visual observers using tape recorders and shortwave time-signal receivers can also make useful contributions. Even simple measurements of the duration of an occultation made with an ordinary stopwatch can be of value. CCD observers should be aware that most of these systems are incapable of timing accuracies better than about 2 s; hence visual observation may be better. Some CCD observers use the trick of turning off the telescope drive shortly before the predicted time and let the images trail. The occultation will appear as a break in the trail that can be measured to about a tenth of a second if the moment the exposure is started (just after turning off the drive) is accurately timed.

Occultation observations are coordinated in North America by the International Occultation Timing Association (IOTA). Whether or not you are an IOTA member, IOTA wants to inform you (and others in your area) of prediction updates, if you are able to observe stars to mag. 11. Please email dunham@starpower.net with the latitude and longitude of proposed observing sites (or location relative to the nearest town), telescope size(s), and an indication of your mobility. Individuals interested in joining IOTA should refer to OCCULTATIONS BY THE MOON (see p. 162), for membership information. More information can be found in the Solar System Photometry Handbook (Willmann-Bell, Inc., 1983), Sky & Telescope, and occasional papers in the Astronomical Journal, Icarus, Minor Planet Bulletin (www.minorplanet.info), and other scientific publications.

246 Planetary Occultations

RASC OBSERVER’S HANDBOOK 2013

Observations of occultations by planetary bodies, including negative observa-tions, should be sent to reports@asteroidoccultation.com for analysis and publication by IOTA. When reporting timings, describe your geographic latitude, longitude, and altitude (to the nearest arcsecond and 30 m, respectively), telescope aperture, timing method, the start and end time of observation, an estimate of the observer’s reac-tion time (if applicable), the accuracy of the timing, and whether the reaction time correction has been applied. The report forms at www.asteroidoccultation.com/observations are preferred; observational results are also posted there, and even more useful information.

Table of Planetary OccultationsThe following two-page table (see p. 248) of planetary occultations, visible from North America and Hawaii in 2013, is based on predictions by Edwin Goffin, Scott Donnell, Steve Preston, Derek Breit, and David Herald. Preston and Breit assisted Dunham and Stamm in the selection for the two-page table, and Paul Maley and Scott Degenhardt also gave some important advice for this work.

The successive columns in the table list: (1) the date and central time (UT) of the event; (2) the occulting body; (3) the apparent magnitude of the body; (4) the catalogue and number of the occulted star; (5) the star’s apparent visual magnitude; (6) the star’s RA and (7) Dec; (8) the expected magnitude change from the combined brightness; (9) the predicted maximum occultation duration in seconds; and (10) the approximate region from which the occultation is predicted to be visible (locations are listed chronologically from first to last). Due to uncertainties in the catalogue positions of the stars and the ephemerides of the minor planetss from which these predictions are derived, the region of visibility of an occultation cannot be refined until CCD observations link the star and minor planet to the new HIPPARCOS reference frame, usually a few weeks prior to the event. Errors still remain, so those near but outside the paths should try to observe. Maps and more information about these events is at www.poyntsource.com/New/RASC_Events.htm.

Note that listed event times are the geocentric time of closest approach; for any specific location in North America or Hawaii, the event time can be several minutes earlier or later. A few weeks before each event, improved predictions and the latest path maps are posted at www.asteroidoccultation.com, Steve Preston’s minor planet occultation website. See www.poyntsource.com/New/Global.htm for additional useful information, including interactive maps to zoom in on the path, circumstances for dozens of stations in and near the path, and lists of stars that can be used to centre telescopes on target stars. Occult Watcher can be used to find other planetary occul-tations visible from your site (www.hristopavlov.net/OccultWatcher/publish.htm). Since Occult Watcher works from an interactive Web site, IOTA uses it to coordinate minor planet occultation observation plans.

Star catalogs are abbreviated as follows: SAO (Smithsonian Astrophysical Observatory), ZC (Robertson Zodiacal Catalog), TYC (Tycho-2), PPM (Roeser Positions and Proper Motions), HIP (Hipparcos), and 2UC (US Naval Observatory UCAC2).

Some event stars, marked by * in the main table, have alternative star numbers, shown in the table on the facing page: Planet # is the dwarf or minor planet number and the alternative star number (Alt. Star #) is from the HIPPARCOS-mission cata-logs used for the predictions on IOTA’s planetary occultation Web sites mentioned above. (Tycho 2 catalog numbers are abbreviated since they all have 0 for the 5th number and 1 for the last, and hyphens are removed; thus, TYC 17810821 is in full, TYC 1781-00821-1.) Spectral types (Sp.) are not available for some of the stars.

RASC OBSERVER’S HANDBOOK 2013

Dwarf anD Minor Planets 247

Noteworthy events (marked in bold type in the main table on next 2 pages):Jan. 2: V573 Persei = SAO 56308 = HIP 15241, spectral type K0, is an eclipsing variable with mag. range

6.11–6.19.

Feb. 4: 129 Antigone is an unusual M-class (with metallic spectral characteristics) minor planet; its shape may be unusual.

Feb. 14: ZC 274 = SAO 110175 = HIP 8655, spectral type M1, angular diameter about 0.7 mas.

Feb. 27 and Mar. 2: Video observations of a 2004 occultation by 98 Ianthe indicate that it may have a satellite.

Apr. 8: SAO 62159 = HIP 51978, spectral type F5. 785 Zwetana is an M-class minor planet (see Feb. 4)

Apr. 18: ZC 865 = SAO 77450 = HIP 26964, spectral type B3.

Jun. 12: ZC 2482 = SAO 185213 = HIP 84478 = V2215 Oph spectral type K2. The star is the distant (separation 732″ in PA 76°) C-companion of 36 Oph (mag. 5), both 19.5 ly distant. Neither 36 Oph nor its close (separation 5″) B component will be occulted. The RS-type variable has range of only 0.08 magnitude, with no period determined.

Jul. 12: SAO 187957 = TYC 6883-00488-1 has an 11.5-mag. companion 8″ away in PA 13° that may be occulted in Antarctica.

Jul. 29: 1074 Beljawskya: SAO 92893 = HIP 10921, spectral type K0, is the preceding component of BD +13° 374. The 10.4-mag. following component is 86″ away and will not be occulted.

Aug. 18: The 4.0″ disk of Mars will be 97% sunlit so the defect of illumination will be an insignificant 0.12″. Good atmospheric seeing will be needed since 1 square arcsecond of Mars will be magnitude 4.3. SAO 79628 = HIP 37579, spectral type F5.

Oct. 11: 2085 Henan: 30 Psc = ZC 3536 = SAO 147042 = HIP 154, a spectral type M3 red giant star about 6 mas across that needs about 0.8 seconds to cover by the advancing edge of Henan. That is more than 1/3 the occultation duration. Of the predicted 19-km path width, only 12 km will have a total occultation of the star, while there will be 7-km-wide partial occultation zones centered on the predicted path limits. Video and CCD observers will need to take care to avoid saturation by the bright star. Success needs observation from several stations since the 1-σ path uncertainty is 1.7 path-widths.

Oct. 12: The 20″ disk of Venus will be 59% sunlit. Only the dark-side disappearance will be seen. SAO 184147 = TYC 6780-01430-1, spectral type Mb.

Oct. 21: The Trojan asteroid 617 Patroclus | Menoetius is binary, with 121-km (Patroclus) and 113-km (Menoetius) components separated by 680 km. Preliminary predictions indicate that the bodies will be approximately aligned with the motion of the pair, so the paths may be close to that predicted for the center of mass given here. If so, their occultations will be time-separated by about 40 s. Since observations will be valuable to determine the parameters of this system, you are invited to join IOTA’s campaign to observe this rare event.

Nov. 10: Observations in 1978 of an occultation of a mag. 6 star show that 532 Herculina may have a satellite about 900 km away.

Nov. 21: The 33″ disk of Venus will be 37% sunlit. Only the dark-side disappearance can be seen. ZC 2781 = SAO 187650 = HIP 93736, spectral type K2.

Jan. 21 679 HIP 51406 F8 26 106 TYC 61710389 A5Feb. 4 150 TYC 62310977 22 469 HIP 25363 F2Mar. 7 329 HIP 71779 F2Jul. 1 1481 HIP 104665 F8 13 501 TYC 06170407 F0 13 1041 HIP 110608 G0 26 387 TYC 57190866 F0

Jul. 29 866 TYC 68980142 Sep. 7 1005 HIP 116629 A2 28 339 TYC 07220353 B9Oct. 6 307 TYC 00300604 G5 18 1186 HIP 100224 F2 29 476 TYC 52000273 F8Nov. 30 709 TYC 11531015 G5 30 355 TYC 18082539 M0Dec. 26 733 HIP 17548 B9

Date Planet # Alt. Star # Sp. Date Planet # Alt. Star # Sp.

Alternative star numbers for some events (*) in the main table (see next 2 pages):

248 Planetary Occultations

RASC OBSERVER’S HANDBOOK 2013

† Ja

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IOTA SELECTED LIST OF NORTH AMERICAN PLANETARY OCCULTATIONS FOR 2013

R

A (

2000

) D

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. 247

.

RASC OBSERVER’S HANDBOOK 2013

Dwarf anD Minor Planets 249

Aug

. 17

7:

03

713

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515

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12

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Mar

s 1.

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1 07

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110

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7

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05 A

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21 4

1 5.

9 2.

9 W

este

rn F

lorid

a >

sout

heas

t New

Bru

nsw

ick

13

2:

26

559

Nan

on

14.1

TY

C 6

877-

0092

0-1

11.4

19

00

14.7

–2

5 14

50

2.8

12.4

C

enra

l Alb

erta

> C

ape

Cod

, Mas

s.

28

8:20

33

9 D

orot

hea

14.7

*S

AO

947

20

8.8

05 3

8 31

.6

+12

40 0

6 5.

9 4.

1 So

uthe

rn O

rego

n >

sout

hern

Mar

ylan

dO

ct.

6 2:

49

307

Nik

e 13

.7

*PPM

145

076

10.6

01

52

41.5

+0

1 12

41

3.2

6.2

Labr

ador

> n

orth

ern

Ariz

ona

6

6:16

11

Par

then

ope

11.7

2U

C 3

8425

933

11.1

07

31

09.9

+1

8 56

27

1.1

7.6

Okl

ahom

a >

Nov

a Sc

otia

6

9:53

22

7 Ph

iloso

phia

15

.1

TYC

193

2-00

850-

1 11

.1

08 2

1 47

.3

+25

16 0

8 4.

0 4.

0 N

orth

ern

Cal

iforn

ia >

New

foun

dlan

d

11

8:21

20

85 H

enan

15

.0

30

Pisc

ium

4.

4 00

01

57.7

–0

6 00

51

10.6

2.

8 N

orth

east

ern

Nor

th C

arol

ina

> Ba

ja S

ur

11

10:4

3 75

1 Fa

ina

13.9

TY

C 1

943-

0042

1-1

10.8

08

45

33.7

+2

4 44

48

3.2

4.9

Baj

a Su

r > so

uthe

rn G

eorg

ia

12

2:06

V

enus

–4

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SAO

184

147

8.8

16 0

8 12

.4

–23

47 3

6

451.

8 M

exic

o >

sout

hwes

tern

U.S

.A.

17

1:

57

173

Ino

12.7

TY

C 6

301-

0076

2-1

9.4

19 2

5 48

.5

–18

21 4

1 3.

3 8.

1 B

aja

Sur >

sout

h of

Flo

rida

17

6:

16

11 P

arth

enop

e 11

.6

TYC

136

5-01

111-

1 10

.8

07 4

2 03

.2

+18

31 2

5 1.

2 9.

7 So

uthe

ast N

ew M

exic

o >

sout

hern

Nov

a Sc

otia

18

3:

18

1186

Tur

nera

14

.4

*SA

O 2

1200

3 7.

3 20

19

37.5

–3

1 43

46

7.1

2.4

Baj

a N

orte

> so

uthe

rn M

anito

ba

21

6:43

61

7 Pa

troc

lus

14.7

TY

C 0

646-

0073

0-1

9.6

02 4

7 58

.8

+14

05 5

9 5.

1 8.

6 N

orth

Car

olin

a >

cent

ral C

alifo

rnia

26

6:

21

17 T

hetis

12

.2

TYC

128

1-00

890-

1 11

.4

05 0

0 12

.0

+15

34 1

9 1.

2 12

.7

Jam

es B

ay >

cen

tral C

alifo

rnia

29

1:

47

476

Hed

wig

13

.3

*PPM

204

819

10.0

21

06

38.9

–0

5 33

34

3.3

10.8

Va

ncou

ver >

nor

ther

n Q

uebe

cN

ov.

10

12:3

2 53

2 H

ercu

lina

10.4

TY

C 0

758-

0131

1-1

10.1

06

39

07.7

+1

3 50

56

0.9

88.2

N

E In

dian

a >

NW

Man

itoba

17

5:

26

607

Jenn

y 14

.8

TYC

189

1-00

489-

1 11

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06 3

1 16

.9

+28

19 0

8 3.

5 9.

8 N

orth

ern

Ont

ario

> c

entra

l Cal

iforn

ia

21

21:3

4 V

enus

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.8

ZC 2

781

7.4

19 0

5 11

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–26

08 2

0

988.

0 so

uthe

aste

rn C

anad

a

24

9:01

52

2 H

elga

14

.1

TYC

128

6-00

493-

1 11

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05 0

9 08

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43 1

1 3.

2 7.

6 Lo

ng Is

land

, New

Yor

k >

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gon

25

9:

30

366

Vin

cent

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13.5

TY

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896-

0203

1-1

11.5

05

16

16.3

+3

8 00

23

2.2

6.8

Sout

heas

tern

Geo

rgia

> n

orth

ern

Cal

iforn

ia

26

10:1

6 13

4 So

phro

syne

11

.6

TYC

286

7-01

816-

1 9.

8 03

49

27.3

+4

0 24

50

2.0

10.8

So

uthe

ast T

exas

> c

entra

l Cal

iforn

ia

30

6:22

70

9 Fr

ingi

lla

14.0

*S

AO

127

853

10.1

22

56

40.9

+0

8 20

36

3.9

8.1

Ore

gon

> no

rther

n In

dian

a

30

12:0

8 35

5 G

abrie

lla

12.9

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AO

762

93

8.5

03 5

2 57

.3

+27

31 2

7 4.

4 2.

6 H

awai

iD

ec.

8 5:

34

776

Ber

beric

ia

11.3

TY

C 1

886-

0104

0-1

10.4

06

21

55.6

+2

7 31

34

1.3

11.8

So

uthe

rn N

ova

Scot

ia >

cen

tral B

ritis

h C

ol.

11

9:

50

231

Vin

dobo

na

14.0

TY

C 2

390-

0113

7-1

10.4

05

23

43.4

+3

0 22

19

3.6

5.2

Virg

inia

> V

anco

uver

15

12

:16

914

Palis

ana

14.0

TY

C 5

462-

0050

1-1

11.5

09

12

18.1

–1

0 02

16

2.6

7.4

Nor

ther

n O

ntar

io >

cen

tral B

aja

16

9:

00

365

Cor

duba

12

.6

TYC

012

0-00

293-

1 11

.4

05 4

5 04

.9

+02

38 3

9 1.

5 10

.1

Sout

hern

Geo

rgia

> B

aja

Nor

te

22

6:22

60

7 Je

nny

14.0

TY

C 1

872-

0206

6-1

10.7

06

02

53.2

+2

7 19

37

3.3

4.5

Hud

son

Bay

> n

orth

ernV

anco

uver

Isla

nd

23

7:21

38

1 M

yrrh

a 13

.3

TYC

074

5-00

242-

1 10

.4

06 3

2 05

.5

+14

40 3

3 3.

0 9.

6 So

uthe

aste

rn N

orth

Car

olin

a >

sout

hern

Ore

gon

24

1:

01

445

Edna

13

.9

TYC

230

5-00

598-

1 10

.6

01 3

7 37

.5

+36

19 1

8 3.

3 7.

5 W

est-c

entra

l Cal

iforn

ia >

wes

tern

Mex

ico

26

5:

20

733

Moc

ia

14.5

*S

AO

390

79

7.2

03 4

5 27

.6

+47

39 3

7 7.

3 8.

0 N

ova

Scot

ia >

Baj

a N

orte

28

13

:24

141

Lum

en

12.4

TY

C 1

950-

0232

0-1

10.6

09

05

39.3

+2

2 34

53

2.0

16.4

So

uthe

ast T

exas

> c

entra

l Cal

iforn

ia

R

A (

2000

) D

ec

Dur

.D

ate

UT

Occ

ultin

g Bo

dy

Mag

. St

ar

Mag

. h

m s

°

′″

∆M

ag.

s N

omin

al P

ath

IOTA SELECTED LIST OF NORTH AMERICAN PLANETARY OCCULTATIONS FOR 2013 (continued)

† Bo

ld =

see

the

note

for t

his e

vent

at t

he b

otto

m o

f p. 2

47

*Se

e th

e al

tern

ate

star

nam

e fo

r thi

s eve

nt a

t the

top

of p

. 247

.