Astrophysics / Astro-Ph.SR

All posts under category "Astrophysics / Astro-Ph.SR"

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Possible explanations of the Maunder minimum from a flux transport dynamo model

Possible explanations of the Maunder minimum from a flux transport dynamo model

: ์„œ๋ก  ๋ถ„์„ ์„œ๋ก ์—์„œ ์ €์ž๋“ค์€ ํƒœ์–‘ ํ™œ๋™ ์ฃผ๊ธฐ ์ค‘ ๊ฐ€์žฅ ์ค‘์š”ํ•œ ํŠน์ง• ์ค‘ ํ•˜๋‚˜์ธ ๋งˆ์šด๋” ์ตœ์†Œ๊ธฐ์— ๋Œ€ํ•ด ์„ค๋ช…ํ•œ๋‹ค. ์ด ๊ธฐ๊ฐ„ ๋™์•ˆ ํƒœ์–‘ ํ‘์  ์ˆ˜๊ฐ€ ํ˜„์ €ํžˆ ๊ฐ์†Œํ–ˆ์œผ๋ฉฐ, ์ด๋Ÿฌํ•œ ์‚ฌ์‹ค์€ ์—ฌ๋Ÿฌ ์—ฐ๊ตฌ์—์„œ ํ™•์ธ๋˜์—ˆ๋‹ค(Ribes & Nesme Ribes, 1993; Hoyt & Schatten, 1996). ํŠนํžˆ, ์–‘ ๊ทน๋ฐ˜๊ตฌ ๋ชจ๋‘์—์„œ ํƒœ์–‘ ํ‘์  ์ˆ˜๊ฐ€ ๊ฑฐ์˜ ์ œ๋กœ์— ๊ฐ€๊นŒ์›Œ์กŒ์œผ๋ฉฐ ๋‚จ๋ฐ˜๊ตฌ์—์„œ๋Š” ๋งˆ์ง€๋ง‰ ๋‹จ๊ณ„์—์„œ ๋ช‡ ๊ฐœ์˜ ํ‘์ ์ด ๋‚˜ํƒ€๋‚ฌ๋‹ค(Ribes & Nesme Ribes, 1993). ์ฝ”์Šค๋ชจ์ œ๋‹‰ ๋™์œ„ ์›์†Œ ๋ฐ์ดํ„ฐ(Beer et al., 1998; Miyah

Model Astrophysics
The Distance of the Gamma-ray Binary 1FGL J1018.6-5856

The Distance of the Gamma-ray Binary 1FGL J1018.6-5856

๋ณธ ๋…ผ๋ฌธ์€ ๊ฐ๋งˆ์„  ์›์ฒœ 1FGL J1018.6 5856์— ๋Œ€ํ•œ ์‹ฌ๋„ ์žˆ๋Š” ๋ถ„์„์„ ์ œ๊ณตํ•œ๋‹ค. ์ด ์›์ฒœ์€ Fermi Large Area Telescope (LAT)๋ฅผ ํ†ตํ•ด ๋ฐœ๊ฒฌ๋˜์—ˆ์œผ๋ฉฐ, ๋‹ค์–‘ํ•œ ์—๋„ˆ์ง€ ๋ฒ”์œ„์—์„œ ๋ณ€๋™์„ฑ์„ ๋ณด์—ฌ์ฃผ์–ด '๊ฐ๋งˆ์„  ์Œ์„ฑ'์œผ๋กœ ๋ถ„๋ฅ˜๋˜์—ˆ๋‹ค. ๊ฐ๋งˆ์„  ์Œ์„ฑ์€ ๊ณ ์งˆ๋Ÿ‰ X ์„  ์Œ์„ฑ๊ณ„๋กœ, ์ด๋“ค ์ค‘ ์ผ๋ถ€๋Š” ๊ฐ๋งˆ์„  ๋ฐฉ์ถœ์ด๋ผ๋Š” ํŠน์ดํ•œ ์„ฑ์งˆ์„ ๊ฐ€์ง„๋‹ค. 1. ๊ฐ๋งˆ์„  ์›์ฒœ์˜ ๋ณ€๋™์„ฑ ๊ฐ๋งˆ์„  ์›์ฒœ 1FGL J1018.6 5856์€ 16.58 ยฑ 0.04 ์ผ ์ฃผ๊ธฐ์˜ ์ง„๋™์„ฑ์„ ๋ณด์—ฌ์ฃผ๋ฉฐ, ์ด๋Š” Swift ๊ด€์ธก์„ ํ†ตํ•ด ํ™•์ธ๋˜์—ˆ๋‹ค. ๋˜ํ•œ, ๋ผ๋””์˜ค ํŒŒ

Astrophysics
The progenitor of a type Ia supernova with a short delay time?

The progenitor of a type Ia supernova with a short delay time?

: HD 49798/RX J0648.0 4418 ์ฒด๊ณ„๋Š” ๋ณ„๋“ค์˜ ํŠน์ดํ•œ ์„ฑ์งˆ๋กœ ์ธํ•ด ์˜ค๋žซ๋™์•ˆ ์ฒœ๋ฌธํ•™์ž๋“ค์˜ ๊ด€์‹ฌ์„ ๋ฐ›์•˜์Šต๋‹ˆ๋‹ค. ์ด ์ฒด๊ณ„์˜ ์ฃผ์š” ๊ตฌ์„ฑ ์š”์†Œ ์ค‘ ํ•˜๋‚˜์ธ HD 49798์€ ๋ฐ๊ณ  ํŒŒ๋ž€์ƒ‰์ด๋ฉฐ, ํ—ฌ๋ฅจ๊ณผ ์งˆ์†Œ์˜ ๋†๋„๊ฐ€ ๋†’์•„ ์กฐ๊ธฐํ˜• ํ•˜์œ„๊ฑฐ์„ฑ์œผ๋กœ ๋ถ„๋ฅ˜๋˜์—ˆ์Šต๋‹ˆ๋‹ค. ์ด๋Ÿฌํ•œ ํŠน์ง•๋“ค์€ HD 49798์ด ์ดˆ๊ธฐ์—๋Š” ๋” ๋ฌด๊ฒ๊ณ  ํฐ ๋ณ„์˜ ํƒˆ๊ฐ๋œ ํ•ต์ผ ๊ฐ€๋Šฅ์„ฑ์„ ์‹œ์‚ฌํ•ฉ๋‹ˆ๋‹ค. 1960๋…„๋Œ€๋ถ€ํ„ฐ HD 49798์— ๋Œ€ํ•œ ๊ด€์ธก๊ณผ ์—ฐ๊ตฌ๊ฐ€ ์ง„ํ–‰๋˜์—ˆ์œผ๋ฉฐ, ํŠนํžˆ 1996๋…„ ROSAT๋ฅผ ํ†ตํ•ด ์ด ๋ณ„์—์„œ ์†Œํ”„ํŠธ X ๋ ˆ์ด ํŽ„์Šค๊ฐ€ ๋ฐœ๊ฒฌ๋˜๋ฉด์„œ ๊ทธ ๋™๋ฐ˜์„ฑ์ด ์••์ถ•๋œ ๋ฌผ์ฒด๋ผ๋Š” ๊ฒƒ์ด

Astrophysics
The Bipolar X-Ray Jet of the Classical T Tauri Star DG Tau

The Bipolar X-Ray Jet of the Classical T Tauri Star DG Tau

DG Tau๋Š” T ํƒ€์šฐ์„ฑ ์ค‘ ํ•˜๋‚˜๋กœ, ์ฃผ๋ณ€์— ๋งŽ์€ ํ•ญ์„ฑ๊ฐ„ ๋ฌผ์งˆ์ด ์กด์žฌํ•˜๋Š” ๊ฒƒ์œผ๋กœ ์•Œ๋ ค์ ธ ์žˆ์Šต๋‹ˆ๋‹ค. ์ด ์—ฐ๊ตฌ์—์„œ๋Š” DG Tau์—์„œ ๊ด€์ฐฐ๋œ X์„  ์ œํŠธ์˜ ํŠน์ง•๊ณผ ๋™์  ๋ณ€ํ™”๋ฅผ ๋ถ„์„ํ•˜์˜€์Šต๋‹ˆ๋‹ค. ํŠนํžˆ, ์ œํŠธ์˜ ๋™ํ–ฅ๊ณผ ์ถฉ๊ฒฉํŒŒ๋กœ ์ธํ•œ ๊ฐ€์Šค์˜ ์—ดํ™” ํ˜„์ƒ์„ ํ™•์ธํ•˜์˜€์œผ๋ฉฐ, ์ด๋Ÿฌํ•œ ํ˜„์ƒ์€ ๋ณ„ ์ฃผ๋ณ€์˜ ๋ฌผ๋ฆฌํ•™์  ๊ณผ์ •์„ ์ดํ•ดํ•˜๋Š”๋ฐ ์ค‘์š”ํ•œ ๋‹จ์„œ๊ฐ€ ๋˜์—ˆ์Šต๋‹ˆ๋‹ค. X์„  ์ œํŠธ์˜ ๊ด€์ฐฐ ๋ฐ ๋ถ„์„ DG Tau์—์„œ ๊ด€์ฐฐ๋œ X์„  ์ œํŠธ๋Š” PA 225๋„ ๋ฐฉํ–ฅ์œผ๋กœ 5 6'๊นŒ์ง€ ํ™•์žฅ๋˜์–ด ์žˆ์Šต๋‹ˆ๋‹ค. ์ด ์—ฐ๊ตฌ์—์„œ๋Š” Chandra ๋ง์›๊ฒฝ์„ ์ด์šฉํ•˜์—ฌ DG Tau๋ฅผ ์ƒ์„ธํžˆ ๊ด€์ฐฐํ•˜์˜€์œผ๋ฉฐ, ํŠนํžˆ

Astrophysics
Analytical Representation for Equations of State of Dense Matter

Analytical Representation for Equations of State of Dense Matter

๋ณธ ๋…ผ๋ฌธ์˜ ์ฃผ์š” ๋ชฉํ‘œ๋Š” ์ค‘์„ฑ์ž ๋ณ„ ๋‚ด๋ถ€์˜ ๋ฐ€๋„ ๋ฌผ์งˆ์— ๋Œ€ํ•œ ์ƒํƒœ ๋ฐฉ์ •์‹(EoS)์„ ๋ถ„์„์ ์œผ๋กœ ํ‘œํ˜„ํ•˜๋Š” ๊ฒƒ์ž…๋‹ˆ๋‹ค. ์ด ์—ฐ๊ตฌ๋Š” ๊ธฐ์กด์˜ ๋ณด๊ฐ„ ๊ธฐ๋ฒ•์ด ์ˆ˜์ •๋œ ์ค‘๋ ฅ ์ด๋ก ์—์„œ ์ œํ•œ์ ์ด๋ผ๋Š” ๋ฌธ์ œ๋ฅผ ํ•ด๊ฒฐํ•˜๊ธฐ ์œ„ํ•ด, 22๊ฐœ์˜ ๋‹ค์–‘ํ•œ EoS์— ๋Œ€ํ•ด ์ •ํ™•ํ•˜๊ณ  ํ†ตํ•ฉ์ ์ธ ๋ถ„์„์  ํ‘œํ˜„์„ ์ œ๊ณตํ•ฉ๋‹ˆ๋‹ค. ์ค‘์„ฑ์ž ๋ณ„์€ ๋งค์šฐ ๋†’์€ ๋ฐ€๋„์™€ ์••๋ ฅ์„ ๊ฐ€์ง„ ์ฒœ์ฒด๋กœ, ๊ทธ ๋‚ด๋ถ€ ์ƒํƒœ๋Š” ์ผ๋ฐ˜ ์ƒ๋Œ€์„ฑ ์ด๋ก (GR)์—์„œ ์ˆ˜์•• ํ‰ํ˜• ๋ฐฉ์ •์‹(TOV ๋ฐฉ์ •์‹)์„ ํ†ตํ•ด ์„ค๋ช…๋ฉ๋‹ˆ๋‹ค. ๊ทธ๋Ÿฌ๋‚˜ ์ˆ˜์ •๋œ ์ค‘๋ ฅ ์ด๋ก ์—์„œ๋Š” TOV ๋ฐฉ์ •์‹์ด ๋‘ ๋ฒˆ์งธ ๋„ํ•จ์ˆ˜๋ฅผ ํฌํ•จํ•˜๋Š” ํ˜•ํƒœ๋กœ ํ‘œํ˜„๋˜๋ฉฐ, ์ด๋Š” ๊ณ ์ฐจ ๋„ํ•จ์ˆ˜๊ฐ€

Astrophysics

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