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研究生:邱惠玲
研究生(外文):Huey-Ling Chiou
論文名稱:早期光譜型恆星的分佈與運動:古德帶分析
論文名稱(外文):The Distribution and Kinematics of Early Type Stars:An Analysis of The Gould Belt
指導教授:傅學海傅學海引用關係
指導教授(外文):Hsieh-Hai Fu
學位類別:碩士
校院名稱:國立臺灣師範大學
系所名稱:地球科學研究所
學門:自然科學學門
學類:地球科學學類
論文種類:學術論文
論文出版年:2002
畢業學年度:90
語文別:英文
論文頁數:90
中文關鍵詞:古德帶銀河運動早期星銀河系依巴羅斯第谷
外文關鍵詞:Gould beltgalactic kinematicsearly type starthe Milky WayHipparcosTycho
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早期光譜型恆星的分佈與運動:古德帶分析
邱惠玲
國立台灣師範大學地球科學研究所天文組
摘要
亮星在天空中的分佈並不均勻。可以發現亮星主要分佈在銀河盤面上,但是另外仍然可以找到一部分星星,它們屬於太陽附近的帶狀結構,這個結構被稱為古德帶(Gould Belt)。
本研究是由Hipparcos星表中,取出光譜型O、B及A0到A5的恆星研究古德帶的分佈與運動性質。
由於銀河盤面上A型星數量眾多,古德帶的A型星分佈不像OB型星一般顯而易見,只能約略看出一個窄帶狀,若以太陽為中心,這些星所處的環狀區域和銀河盤面的夾角約為16.5度,長軸指向l = 38∘與218∘的方向。除此之外,結合三角視差、自行與徑向速度等觀測數據,可以求得太陽相對於OB型星及A0到A5型恆星的特有運動之速度分量。不論古德帶成因和高速雲或是爆炸事件相關,在速度分佈圖中,應該都可以依據古德帶恆星和銀河盤面恆星運動性質,區分出部分古德帶的成員,改善位置分佈圖中成員星和銀河盤面星星相混雜而難以區別的困境。雖然OB型星能明確的反應古德帶的空間分佈,但在可見光波段也確實可以使用至A5型星來研究。如果早期星有助於研究古德帶邊緣區域,那麼,使用至晚期星應該更能了解古德帶大尺度的分佈及特性。此外,根據運動特性、空間速度及自行速度的差異,能有效突顯古德帶特質。依此,本研究發現O型星和B型星在自行的分佈圖中可用肉眼看見兩個群體,其中一群應該與古德帶相關。

The Distribution and Kinematics of Early Type Stars:
An Analysis of The Gould Belt
Huey-Ling Chiou
Department of Earth Sciences, National Taiwan Normal University
Abstract
The distribution of the brightest stars on the sky looks like a great circle, known as Gould belt from Gould’s research about one century ago. From Hipparcos catalogue and the database enclosed, some early type stars, O, B, and A0 - A5, are selected to analyze to fit the Gould Belt. The distribution and kinematics of these selected stars are used to find information of Gould Belt.
Because the amounts of A type stars spreading on the galactic plane are much more than those O and B type stars, the Gould Belt is not obviously seen. From the distribution of the stars, the Gould Belt likely forms a ring region which is a flat inclining about 16.5 degree to the galactic plane and whose major axis is in the direction of l = 38 degree and 218 degree. In addition, the parallax, proper motion, and radial velocity are combined to find the solar motion with respect to OB stars and A0-A5 stars. Whether the Gould Belt was formed in the explosive event or in the impact event of a high velocity cloud, the members of the Gould Belt should still reserve several information of the velocity, which is different from that of the disk stars. Therefore, the property of the Gould Belt could be found out according to the different kinematical character. The Gould belt could be reflected by space position usually for OB stars, however, the Gould belt is also reflected roughly for main sequence stars with spectral down to A5. If the edge of the Gould Belt could be indexed by early type stars, the late type stars might be used to index larger scale understanding of the Gould Belt. Furthermore, the kinematical characteristic, proper motion or space velocity, is helpful to stand out the Gould Belt in the research. Two groups are seen clearly by eyes from the proper motion vector point diagrams of OB stars, and one could be with relation to the Gould Belt.

Contents
Introduction ------------------------------------------------------------------------------ 1
The investigation of the Gould Belt ------------------------------------------ 1
The distribution of the Gould Belt -------------------------------------------- 4
The origin of the Gould Belt ---------------------------------------------------- 6
The motion and the relation between the Gould Belt and Oort’s constant 6
This work ------------------------------------------------------------------------- 7
Data source -------------------------------------------------------------------------------- 9
Hipparcos Catalogue ------------------------------------------------------------- 9
Radial velocities ----------------------------------------------------------------- 9
Selected criteria ----------------------------------------------------------------------- 11
Analyzing process ------------------------------------------------------------------------ 15
Result -------------------------------------------------------------------------------------- 17
Conclusion -------------------------------------------------------------------------------- 26
Reference --------------------------------------------------------------------------------- 72
Appendix --------------------------------------------------------------------------------- 75
LSR and solar motion ------------------------------------------------------------- 75
Differential rotation (Oort’s constants)------------------------------------------ 75
The transition from the equatorial system to the galactic system ----------- 79
Tables
Table 1: The inclination and deflection of the Gould Belt -------------------------- 4
Table 2: The parameters of the Gould Belt --------------------------------------------- 5
Table 3: The result of Hipparcos and Tycho catalogues ------------------------------ 9
Table 4: The average and errors of radial velocity, parallax, and proper motion--- 13
Table 5: The central groups on the vector point diagram ----------------------------- 18
Table 6: Results of the solar motion ---------------------------------------------------- 22
Table 7: The Oort’s constants ------------------------------------------------------------ 24
Table 8: The result from other published papers -------------------------------------- 24
Figures
Fig. 1 : The diagram of the Gould Belt projected on the XY-plane drawn
from Guillout et al. (1998) ------------------------------------------------------ 3
Fig. 2 : The XYZ distribution of the 8331 OB stars without Rv data in 1000 pc
------------------------------------------------------- 26
Fig. 3 : The XYZ distribution of the 3432 OB stars with Rv data in 1000 pc
------------------------------------------------------- 27
Fig. 4 : The XYZ distribution of the OB stars without Rv data in 1000
pc and sp/p £ 50% ----------------------------------------------------- 28
Fig. 5 : Fig. 5: The XYZ distribution of the OB stars with Rv data in 1000
pc and sp/p £ 50% --------------------------------------------------- 29
Fig. 6 : The XYZ distribution of A0—A5 main sequence stars without Rv
data in 1000pc ------------------------------------------------------ 30
Fig. 7 : The XYZ distribution of A0—A5 main sequence stars with Rv data
in 1000pc --------------------------------------------------- 31
Fig. 8 : The XYZ distribution of the A0-A5V stars without Rv data in 1000 pc
and sp/p £ 50% ------------------------------------------------- 32
Fig. 9 : The XYZ distribution of the A0-A5V stars with Rv data in 1000 pc
and sp/p £ 50% ------------------------------------------------- 33
Fig.10 : The proper motion vector point diagram of OB stars without Rv data
--------------------------------------------------- 34
Fig.11 : The velocity of OB stars without Rv data
-------------------------------------------------- 34
Fig.12-a: Group D divided from the Vl, Vb distribution of the OB stars
without Rv data --------------------------------------------------- 35
Fig.12-b: Group C divided from the Vl, Vb distribution of OB stars
without Rv data. --------------------------------------------------- 36
Fig.12-c: Group D divided from the Vl, Vb distribution of the OB stars
with Rv data --------------------------------------------------- 37
Fig.12-d: Group C divided from the Vl, Vb distribution of OB stars
with Rv data. --------------------------------------------------- 38
Fig.13-a: Group B divided from the mlcosb, mb distribution of OB stars
without Rv data. --------------------------------------------------- 39
Fig.13-b: Group A divided from the mlcosb, mb distribution of OB stars
without Rv data. --------------------------------------------------- 40
Fig.13-c: The XYZ distribution of the A0 — A5 stars without Rv data separated
from mlcosb, mb --------------------------------------------------- 41
Fig.13-d: Group A divided from the mlcosb, mb distribution of OB stars
with Rv data. --------------------------------------------------- 42
Fig.14 : The proper motion vector point diagram of the A0V—A5V stars
without Rv data --------------------------------------------------- 43
Fig.15 : The velocity of the A0V — A5V stars without Rv data
--------------------------------------------------- 43
Fig.16 : The proper motion vector point diagram of the A0V—A5V stars
without Rv data (sp/p £ 50%)------------------------------------------------ 44
Fig.17 : The velocity of the A0V — A5V stars without Rv data (sp/p £ 50%)
-------------------------------------------------- 44
Fig.18-a: The XYZ distribution of the A0 — A5 stars with Rv data and
separated from mlcosb, mb ------------------------------------------------- 45
Fig.18-b: The XYZ distribution of the A0 — A5 stars without Rv data and
separated from mlcosb, mb ------------------------------------------------- 46
Fig.19-a: The XYZ distribution of the A0 — A5 stars without Rv data and
separated from Vl, Vb ------------------------------------------------ 47
Fig.19-b: The XYZ distribution of the A0 — A5 stars with Rv data and
separated from Vl, Vb ------------------------------------------------ 48
Fig.20 : The UVW distribution of the OB stars in 1000 pc
---------------------------------------------------- 49
Fig.21 : The UVW distribution of the OB stars belonging to group D
---------------------------------------------------- 50
Fig.22 : The UVW distribution of the A0-A5 stars belonging to group D
---------------------------------------------------- 51
Fig.23-a: The UVW distribution of the OB stars which is the group B
divided by the mlcosb, mb diagram.------------------------------------------- 52
Fig.23-b: The UVW distribution of the OB stars which is the group A
divided by the mlcosb, mb diagram-------------------------------------------- 53
Fig.24-a: The UVW distribution of the OB stars which is the group D
divided by the Vl, Vb diagram -------------------------------------------- 54
Fig.24-b: The UVW distribution of the OB stars which is the group C
divided by the Vl, Vb diagram -------------------------------------------- 55
Fig.25 : The XYZ diagram of the OB stars whose U, V, and W are negative
--------------------------------------------- 56
Fig.26 : The UVW diagram of the A0 — A5 stars
-------------------------------------------- 57
Fig.27-a: The UVW distribution of the A0-A5 stars which is the group B
divided by the mlcosb, mb diagram----------------------------------------- 58
Fig.27-b: The UVW distribution of the A0-A5 stars which is the group A
divided by the mlcosb, mb diagram ---------------------------------------- 59
Fig.28-a: The UVW distribution of the A0-A5 stars which is the group C
divided by the Vl, Vb diagram ----------------------------------------- 60
Fig.28-b: The UVW distribution of the A0-A5 stars which is the group D
divided by the Vl, Vb diagram ------------------------------------------- 61
Fig.29 : The UVW diagram of the selected OB stars (sp/p £ 50%)
-------------------------------------------- 62
Fig.30 : The UVW of the A0V ~ A5V stars with sp/p £ 50%
----------------------------------------------- 63
Fig. 31 : The XYZ distribution of the OB stars in the Gould Belt coordinate
which is from the model of Guillout et al. (1998)----------------------------- 64
Fig. 32 : The XYZ distribution of the OB stars in the Gould Belt coordinate
which is from the model of Olano (1982) ----------------------------------- 65
Fig. 33 : The XYZ distribution of the OB stars in the Gould Belt coordinate
which is from the model of Lindblad et al. (1973) -------------------------- 66
Fig. 34: The XYZ diagram of the OB stars with sp/p £ 50% from the model of
Guillout et al. (1998) -------------------------------------------- 67
Fig. 35: The XYZ diagram of the A0V ~ A5V stars with sp/p £ 50%
from the model of Guillout et al. (1998) ---------------------------------- 68
Fig. 36: The XYZ diagram of the OB stars with sp/p £ 50% transferred to the
result in the work ------------------------------------------ 69
Fig. 37: The XYZ diagram of the A0V~A5V stars with sp/p£50% transferred
to the result in the work ------------------------------------------ 70

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