사용자:Ta183ta/연습장: 두 판 사이의 차이
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'''호문쿨루스 성운'''(Homunculus Nebula)은 지구로부터 용골자리 방향으로 약 7500 광년(약 2300 파섹) 떨어져 있는 쌍극성 발광성운이자 반사성운으로 무거운 항성계 용골자리 에타를 둘러싸고 있다. 이 성운은 항성이 생성되는 H II 영역이자 자기보다 훨씬 더 큰 용골자리 성운 안에 있다. 이름의 유래는 라틴어로 '작은 사람'을 뜻하는 호문쿨루스 ''homunculus'' 이며 성운을 구성하는 가스는 1841년 용골자리 에타에서 분출된 것이다.<ref name=teodoro>{{cite journal|bibcode=2008MNRAS.387..564T|title=Near-infrared integral field spectroscopy of the Homunculus nebula around η Carinae using Gemini/CIRPASS|journal=Monthly Notices of the Royal Astronomical Society|volume=387|issue=2|pages=564|author1=Teodoro|first1=M.|last2=Damineli|first2=A.|last3=Sharp|first3=R. G.|last4=Groh|first4=J. H.|last5=Barbosa|first5=C. L.|year=2008|doi=10.1111/j.1365-2966.2008.13264.x|arxiv = 0804.0240 }}</ref> 성운에 포함되어 있는 먼지는 극도로 광도가 높은 중앙 항성계에서 발산되는 빛의 대부분을 흡수하여 이를 다시 적외선 형태로 복사한다. 호문쿨루스 성운은 중적외선 파장으로 한정시 밤하늘에서 가장 밝은 천체이다.<ref name=imposters>{{cite book|doi=10.1007/978-1-4614-2275-4_7|chapter=All Things Homunculus|title=Eta Carinae and the Supernova Impostors|journal=Eta Carinae and the Supernova Impostors|volume=384|pages=145|series=Astrophysics and Space Science Library|year=2012|last1=Smith|first1=Nathan|isbn=978-1-4614-2274-7|bibcode=2012ASSL..384..145S}}</ref> |
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호문쿨루스 성운 안에는 '작은 호문쿨루스'''Little Homunculus'' 가 있다. 작은 호문쿨루스 안에는 다시 '아기 호문쿨루스' ''Baby Homunculus'' 가 있는데 이는 항성풍에 의해 충격을 받은 물질로 된 껍질 구조이다.<ref name=abraham/> |
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==관측 역사== |
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==Observational history== |
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1914년 관측기록에서 용골자리 에타는 희미한 동반천체 하나를 거느리고 있으며 이 천체는 항성이 아닌 것으로 보고되었다.<ref name=innes>{{cite journal|bibcode=1914MNRAS..74..697I|title=Η Argûs, Magnitude of, in 1914, and the discovery of a close companion to it|journal=Monthly Notices of the Royal Astronomical Society|volume=74|issue=8|pages=697|author1=Innes|first1=R. T. A.|year=1914|doi=10.1093/mnras/74.8.697}}</ref> 1944년과 1945년에는 폭 5", 길이 10" 정도로 약간 길쭉한 모양의 성운 구조가 관측되었는데 이 성운은 It was measured to be expanding at a rate which was consistent with having originated in an explosion in the mid 19th century. At that time the shape of the nebula showed a central bulge with a single large lump to the northwest and two smaller extensions to the southeast, which was described as a ''Homunculus''.<ref name=gaviola>{{cite journal|bibcode=1950ApJ...111..408G|title=Eta Carinae. I. The Nebulosity|journal=Astrophysical Journal|volume=111|pages=408|author1=Gaviola|first1=E.|year=1950|doi=10.1086/145274}}</ref> Other observations at around the same time described a strongly orange central region in a larger fainter green nebulosity. One paper described it as looking like a "red spade-beard".<ref name=thackeray>{{cite journal|bibcode=1949Obs....69...31T|title=Nebulosity surrounding eta Carinae|journal=The Observatory|volume=69|pages=31|author1=Thackeray|first1=A. D.|year=1949}}</ref> |
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==모양== |
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[[File:3D Homunculus Nebula.jpg|left|thumb|upright=1.2| |
[[File:3D Homunculus Nebula.jpg|left|thumb|upright=1.2|호문쿨루스 성운의 3D 모형.]] |
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The Homunculus consists of two lobes, referred to as northwest (NW) and southeast (SE) based on their orientation as seen from Earth. |
The Homunculus consists of two 엽(葉)lobes, referred to as northwest (NW) and southeast (SE) based on their orientation as seen from Earth. 두 엽 모두 너비는 {{val|7|u="}}, 길이는 {{val|5|u="}} 정도이다. There is also a ragged equatorial skirt of material which can be seen faintly in deep images at certain wavelengths. The lobes are mostly hollow with the material strongly concentrated towards the poles.<ref name=abraham/><ref name=steffen/> |
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The equatorial skirt appears to contain material of the same age and younger than the lobes. It contains a much smaller mass of material than the lobes, shining mainly by reflected light which escapes most easily at equatorial latitudes. There is less dust and little molecular hydrogen compared to the lobes.<ref name=smith2006>{{cite journal|doi=10.1086/503766|title=The Structure of the Homunculus. I. Shape and Latitude Dependence from H2and [Feii] Velocity Maps of η Carinae|journal=The Astrophysical Journal|volume=644|issue=2|pages=1151|year=2006|last1=Smith|first1=Nathan|bibcode=2006ApJ...644.1151S|arxiv = astro-ph/0602464 }}</ref> |
The equatorial skirt appears to contain material of the same age and younger than the lobes. It contains a much smaller mass of material than the lobes, shining mainly by reflected light which escapes most easily at equatorial latitudes. There is less dust and little molecular hydrogen compared to the lobes.<ref name=smith2006>{{cite journal|doi=10.1086/503766|title=The Structure of the Homunculus. I. Shape and Latitude Dependence from H2and [Feii] Velocity Maps of η Carinae|journal=The Astrophysical Journal|volume=644|issue=2|pages=1151|year=2006|last1=Smith|first1=Nathan|bibcode=2006ApJ...644.1151S|arxiv = astro-ph/0602464 }}</ref> |
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| 48번째 줄: | 48번째 줄: | ||
The reflected spectrum of the Homunculus lobes varies with position, due to the central star emitting different radiation at different latitudes on its surface. This is the only star for which such an effect can be observed.<ref name="smith2006"/> |
The reflected spectrum of the Homunculus lobes varies with position, due to the central star emitting different radiation at different latitudes on its surface. This is the only star for which such an effect can be observed.<ref name="smith2006"/> |
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==생성== |
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{{main| |
{{main|용골자리 에타}} |
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호문쿨루스 성운은 용골자리 에타가 일으킨 막대한 폭발로 뿜어져 나온 물질이다. 이 사건에서 방출된 빛은 1841년 지구에 도달했으며 이 때 용골자리 에타는 밤하늘에서 시리우스 다음으로 밝은 항성이 되었다. 그러나 별에서 분출된 기체와 먼지는 이후 별의 빛 대부분을 차단했다. 이 의사 초신성 폭발은 극엽(極葉) 두 개와 거대하지만 얇은 적도 원반 하나를 만들었으며 이 구조들은 모두 초당 670 킬로미터 속도로 확산되고 있다. |
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The Homunculus was ejected in an enormous outburst from Eta Carinae. Light from this event reached Earth in 1841, when Eta Carinae briefly became the second-brightest star in the sky, after [[Sirius]]; the ejected gas and dust have since obscured much of its light. The [[Supernova imposter|near-supernova]] explosion produced two polar lobes, and a large but thin [[Non-inclined orbit|equatorial]] disk, all moving outward at up to {{convert|670|km/s|mph|abbr=on}}. |
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The Homunculus Nebula is a virtually unique structure, believed to result from the extremely young age. This means that the shape and structure is almost entirely due to the original eruption rather than the interaction with surrounding interstellar material. Suggestions that the waist between the two lobes was formed by "pinching" from a dense surrounding material have been disproved, and the bipolar shells are now believed to be caused by concentrated polar outflows of material, with the equatorial skirt formed by breakout of faster ejected material through the thinnest parts of the shells.<ref name=steffen/> The ejection of material preferentially along the axis of rotation of the stars, or of the binary orbit, may be due to the rotation of Eta Carinae A itself resulting in stronger mass loss towards the poles.<ref name=smith2006/> |
The Homunculus Nebula is a virtually unique structure, believed to result from the extremely young age. This means that the shape and structure is almost entirely due to the original eruption rather than the interaction with surrounding interstellar material. Suggestions that the waist between the two lobes was formed by "pinching" from a dense surrounding material have been disproved, and the bipolar shells are now believed to be caused by concentrated polar outflows of material, with the equatorial skirt formed by breakout of faster ejected material through the thinnest parts of the shells.<ref name=steffen/> The ejection of material preferentially along the axis of rotation of the stars, or of the binary orbit, may be due to the rotation of Eta Carinae A itself resulting in stronger mass loss towards the poles.<ref name=smith2006/> |
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| 58번째 줄: | 58번째 줄: | ||
Analysis of the expansion of the nebula has given a time for its formation at {{val|1847.1|0.8|ul=yr|fmt=none}}. This date is inconsistent with the peaks in brightness and with estimates of the [[periastron]] passage of the secondary star.<ref name=smith>{{cite journal|bibcode=2017MNRAS.471.4465S|title=A moderately precise dynamical age for the Homunculus of Eta Carinae based on 13 years of HST imaging|journal=Monthly Notices of the Royal Astronomical Society|volume=471|issue=4|pages=4465–4475|last1=Smith|first1=Nathan|year=2017|arxiv=1709.06210|doi=10.1093/mnras/stx1868}}</ref> |
Analysis of the expansion of the nebula has given a time for its formation at {{val|1847.1|0.8|ul=yr|fmt=none}}. This date is inconsistent with the peaks in brightness and with estimates of the [[periastron]] passage of the secondary star.<ref name=smith>{{cite journal|bibcode=2017MNRAS.471.4465S|title=A moderately precise dynamical age for the Homunculus of Eta Carinae based on 13 years of HST imaging|journal=Monthly Notices of the Royal Astronomical Society|volume=471|issue=4|pages=4465–4475|last1=Smith|first1=Nathan|year=2017|arxiv=1709.06210|doi=10.1093/mnras/stx1868}}</ref> |
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==거리== |
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[[File:Eta Carinae (HST).jpg|left|thumb| |
[[File:Eta Carinae (HST).jpg|left|thumb|용골자리 에타 주변의 호문쿨루스 성운.(HST UV, 가시광선 사진)]] |
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The Homunculus and Eta Carinae are assumed to be at approximately the same distance as Trumpler 16 and the Carina Nebula, but the distances to these objects are not known with any great accuracy. Instead, the distance of the Homunculus Nebula itself can be calculated using measurements of its expansion. The velocity of particular locations within the thin shell of the Homunculus lobes can be measured using the [[doppler shift]] of the spectral lines at that point, assuming the lobes are symmetrical. There are two different doppler shifts visible in the spectrum: one for direct emission lines; and one for reflected lines from Eta Carinae A. The direct line doppler shift gives the expansion velocity of the shell project onto the line of sight. Assuming an origin in Eta Carinae's Great Eruption and a constant expansion velocity, this gives the linear distance of the shell from the central star projected along the line of sight. The difference between the reflected line doppler shift velocity and the direct line velocity gives the distance of the shell from the central star, again assuming expansion at constant velocity since the Great Eruption. |
The Homunculus and Eta Carinae are assumed to be at approximately the same distance as Trumpler 16 and the Carina Nebula, but the distances to these objects are not known with any great accuracy. Instead, the distance of the Homunculus Nebula itself can be calculated using measurements of its expansion. The velocity of particular locations within the thin shell of the Homunculus lobes can be measured using the [[doppler shift]] of the spectral lines at that point, assuming the lobes are symmetrical. There are two different doppler shifts visible in the spectrum: one for direct emission lines; and one for reflected lines from Eta Carinae A. The direct line doppler shift gives the expansion velocity of the shell project onto the line of sight. Assuming an origin in Eta Carinae's Great Eruption and a constant expansion velocity, this gives the linear distance of the shell from the central star projected along the line of sight. The difference between the reflected line doppler shift velocity and the direct line velocity gives the distance of the shell from the central star, again assuming expansion at constant velocity since the Great Eruption. |
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| 66번째 줄: | 66번째 줄: | ||
The same calculations also return the inclination of the axis of the Homunculus relative to the line of sight. This turns out to be 41°, or 49° relative to the plane of the sky, which means it is slightly more "end on" than "side on".<ref name=smith2006/><ref name=davidson/> |
The same calculations also return the inclination of the axis of the Homunculus relative to the line of sight. This turns out to be 41°, or 49° relative to the plane of the sky, which means it is slightly more "end on" than "side on".<ref name=smith2006/><ref name=davidson/> |
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==각주== |
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2020년 4월 23일 (목) 16:55 판
| 호문쿨루스 성운 | |
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| 관측 정보 | |
|---|---|
| 형태 | 발광/반사성운 |
| 적경 | 10h 45m 03.6s[1] |
| 적위 | -59° 41′ 04″[1] |
| 거리 | 7500 광년 |
| 겉보기 등급 | 6.21 (-0.8–7.9) (중심별 포함) |
| 별자리 | 용골자리 |
| 물리적 성질 | |
| 반지름 | 0.29 광년[2](18"[2]) |
| 특이사항 | 쌍극성운 |
| 메시에 천체 목록 NGC 천체 목록 | |
호문쿨루스 성운(Homunculus Nebula)은 지구로부터 용골자리 방향으로 약 7500 광년(약 2300 파섹) 떨어져 있는 쌍극성 발광성운이자 반사성운으로 무거운 항성계 용골자리 에타를 둘러싸고 있다. 이 성운은 항성이 생성되는 H II 영역이자 자기보다 훨씬 더 큰 용골자리 성운 안에 있다. 이름의 유래는 라틴어로 '작은 사람'을 뜻하는 호문쿨루스 homunculus 이며 성운을 구성하는 가스는 1841년 용골자리 에타에서 분출된 것이다.[3] 성운에 포함되어 있는 먼지는 극도로 광도가 높은 중앙 항성계에서 발산되는 빛의 대부분을 흡수하여 이를 다시 적외선 형태로 복사한다. 호문쿨루스 성운은 중적외선 파장으로 한정시 밤하늘에서 가장 밝은 천체이다.[4]
호문쿨루스 성운 안에는 '작은 호문쿨루스'Little Homunculus 가 있다. 작은 호문쿨루스 안에는 다시 '아기 호문쿨루스' Baby Homunculus 가 있는데 이는 항성풍에 의해 충격을 받은 물질로 된 껍질 구조이다.[2]
관측 역사
1914년 관측기록에서 용골자리 에타는 희미한 동반천체 하나를 거느리고 있으며 이 천체는 항성이 아닌 것으로 보고되었다.[5] 1944년과 1945년에는 폭 5", 길이 10" 정도로 약간 길쭉한 모양의 성운 구조가 관측되었는데 이 성운은 It was measured to be expanding at a rate which was consistent with having originated in an explosion in the mid 19th century. At that time the shape of the nebula showed a central bulge with a single large lump to the northwest and two smaller extensions to the southeast, which was described as a Homunculus.[6] Other observations at around the same time described a strongly orange central region in a larger fainter green nebulosity. One paper described it as looking like a "red spade-beard".[7]
모양
The Homunculus consists of two 엽(葉)lobes, referred to as northwest (NW) and southeast (SE) based on their orientation as seen from Earth. 두 엽 모두 너비는 7″, 길이는 5″ 정도이다. There is also a ragged equatorial skirt of material which can be seen faintly in deep images at certain wavelengths. The lobes are mostly hollow with the material strongly concentrated towards the poles.[2][8]
The equatorial skirt appears to contain material of the same age and younger than the lobes. It contains a much smaller mass of material than the lobes, shining mainly by reflected light which escapes most easily at equatorial latitudes. There is less dust and little molecular hydrogen compared to the lobes.[9]
The bipolar nebula is angled so that the NW lobe is further away from Earth than the SE lobe is. The whole nebula is expanding so that the SE lobe is blue-shifted and the NW lobe is red-shifted, relative to the central source. The lobes contain the majority of the material in the Homunculus Nebula, in relatively thin shells concentrated towards the poles. The shells consist of two components, an inner warm region and a more massive outer cool skin. The shells are smooth and thin suggesting they were ejected in as little as five years, but there are streaks of thicker dust detectable within the shells.[9]
Each lobe has polar "hole" although it is not known whether it is an actual gap in the shell of the lobe or just a deep indentation. Surrounding each polar hole is a "trench". The trenches are visible as approximate semicircles centred on the axis of the lobes but may form complete circles. There are other smaller irregular indentations and protrusions to the lobes, which are symmetrical with the same features appearing on each lobe. These include flattened protrusions at about 10° latitude, [모호한 표현] one on each lobe, with other smaller protrusions near the equatorial skirt.[8]
The mass of the nebula cannot be determined directly. However, the amount of dust can be measured fairly accurately and estimates of the gas to dust ratio used to calculate the total mass. The total dust mass is calculated at 틀:Solar mass, leading to estimates that up to 틀:Solar mass of gas are contained in the Homunculus itself. Nearly as much material is detected within outer ejecta, which formed earlier, but within the last thousand years. Older calculations had produce consensus estimates of 틀:Solar mass[11]
Weigelt Blobs
Early speckle interferometry showed that the central region of the Homunculus contains four point-like sources, originally designated A1, A2, A3, and A4.[12] The four speckle objects were later referred to as A, B, C, and D. Higher resolution studies showed that only the brightest source A was truly stellar, and the other three were small nebular condensations. The three Weigelt Blobs are visible primarily in light directly reflected from the Eta Carinae stars. The blobs are believed to lie near the equatorial plane of the stellar system, but their origin is unclear. Their speed has been measured, but within uncertainties they could have been emitted in the 1890 outburst or a 1941 event. The situation is complicated further by the likely acceleration of their slow movement due to the intense stellar winds.[13]
Spectrum
The spectrum of the Homunculus is complex, consisting of reflected, thermal, and emission components at wavelengths across the electromagnetic spectrum. The dominant feature is blackbody radiation from dust heated by the stars within. Overlaid on this is some light from the stars themselves reflected mostly from dense features within the nebulosity, showing strong visual and UV spectral lines in emission. There are also emission lines from ionised gas where it collides with slower moving material or is excited by high energy electromagnetic radiation from the stars. The ionisation emission is similar to a planetary nebula but at lower levels of ionisation due to the lower temperatures of the central stars. The strongest lines are [Fe ii] and [N ii], similar to those from the stellar winds of the stars themselves, but with narrower profiles.[9]
Shock waves at the outer edge of the ejecta are heated to millions of kelvin and emit x-ray radiation. The lobes of the Homunculus emit copious radio waves, including emission in the 21 cm line of hydrogen.
The reflected spectrum of the Homunculus lobes varies with position, due to the central star emitting different radiation at different latitudes on its surface. This is the only star for which such an effect can be observed.[9]
생성
이 부분의 본문은 용골자리 에타입니다.호문쿨루스 성운은 용골자리 에타가 일으킨 막대한 폭발로 뿜어져 나온 물질이다. 이 사건에서 방출된 빛은 1841년 지구에 도달했으며 이 때 용골자리 에타는 밤하늘에서 시리우스 다음으로 밝은 항성이 되었다. 그러나 별에서 분출된 기체와 먼지는 이후 별의 빛 대부분을 차단했다. 이 의사 초신성 폭발은 극엽(極葉) 두 개와 거대하지만 얇은 적도 원반 하나를 만들었으며 이 구조들은 모두 초당 670 킬로미터 속도로 확산되고 있다.
The Homunculus Nebula is a virtually unique structure, believed to result from the extremely young age. This means that the shape and structure is almost entirely due to the original eruption rather than the interaction with surrounding interstellar material. Suggestions that the waist between the two lobes was formed by "pinching" from a dense surrounding material have been disproved, and the bipolar shells are now believed to be caused by concentrated polar outflows of material, with the equatorial skirt formed by breakout of faster ejected material through the thinnest parts of the shells.[8] The ejection of material preferentially along the axis of rotation of the stars, or of the binary orbit, may be due to the rotation of Eta Carinae A itself resulting in stronger mass loss towards the poles.[9]
The thinness of the bipolar shells argues for their ejection within approximately five years.[9] Irregularities in the otherwise very smooth structure of the shells are conjectured to result from interactions between the winds of the two central stars, and from their orbital motion.[8]
Analysis of the expansion of the nebula has given a time for its formation at 1847.1±0.8 yr. This date is inconsistent with the peaks in brightness and with estimates of the periastron passage of the secondary star.[14]
거리
The Homunculus and Eta Carinae are assumed to be at approximately the same distance as Trumpler 16 and the Carina Nebula, but the distances to these objects are not known with any great accuracy. Instead, the distance of the Homunculus Nebula itself can be calculated using measurements of its expansion. The velocity of particular locations within the thin shell of the Homunculus lobes can be measured using the doppler shift of the spectral lines at that point, assuming the lobes are symmetrical. There are two different doppler shifts visible in the spectrum: one for direct emission lines; and one for reflected lines from Eta Carinae A. The direct line doppler shift gives the expansion velocity of the shell project onto the line of sight. Assuming an origin in Eta Carinae's Great Eruption and a constant expansion velocity, this gives the linear distance of the shell from the central star projected along the line of sight. The difference between the reflected line doppler shift velocity and the direct line velocity gives the distance of the shell from the central star, again assuming expansion at constant velocity since the Great Eruption.
Observations of the spectrum of the Homunculus at a particular angular distance from the central star has shown the actual linear distance of that point from the central star, which defines the distance. Values obtained using this method are around 2.3 kpc with a margin of error around 100 pc.[14][9][15]
The same calculations also return the inclination of the axis of the Homunculus relative to the line of sight. This turns out to be 41°, or 49° relative to the plane of the sky, which means it is slightly more "end on" than "side on".[9][15]
각주
- ↑ 가 나 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). “The Tycho-2 catalogue of the 2.5 million brightest stars”. 《Astronomy and Astrophysics》 355: L27. Bibcode:2000A&A...355L..27H. doi:10.1888/0333750888/2862.
- ↑ 가 나 다 라 Abraham, Zulema; Falceta-Gonçalves, Diego; Beaklini, Pedro P. B. (2014). “Η Carinae Baby Homunculus Uncovered by A/km/kmLMA”. 《The Astrophysical Journal》 791 (2): 95. arXiv:1406.6297. Bibcode:2014ApJ...791...95A. doi:10.1088/0004-637X/791/2/95.
- ↑ Teodoro, M.; Damineli, A.; Sharp, R. G.; Groh, J. H.; Barbosa, C. L. (2008). “Near-infrared integral field spectroscopy of the Homunculus nebula around η Carinae using Gemini/CIRPASS”. 《Monthly Notices of the Royal Astronomical Society》 387 (2): 564. arXiv:0804.0240. Bibcode:2008MNRAS.387..564T. doi:10.1111/j.1365-2966.2008.13264.x.
- ↑ Smith, Nathan (2012). 〈All Things Homunculus〉. 《Eta Carinae and the Supernova Impostors》. 《Eta Carinae and the Supernova Impostors》. Astrophysics and Space Science Library 384. 145쪽. Bibcode:2012ASSL..384..145S. doi:10.1007/978-1-4614-2275-4_7. ISBN 978-1-4614-2274-7.
- ↑ Innes, R. T. A. (1914). “Η Argûs, Magnitude of, in 1914, and the discovery of a close companion to it”. 《Monthly Notices of the Royal Astronomical Society》 74 (8): 697. Bibcode:1914MNRAS..74..697I. doi:10.1093/mnras/74.8.697.
- ↑ Gaviola, E. (1950). “Eta Carinae. I. The Nebulosity”. 《Astrophysical Journal》 111: 408. Bibcode:1950ApJ...111..408G. doi:10.1086/145274.
- ↑ Thackeray, A. D. (1949). “Nebulosity surrounding eta Carinae”. 《The Observatory》 69: 31. Bibcode:1949Obs....69...31T.
- ↑ 가 나 다 라 Steffen, W.; Teodoro, M.; Madura, T. I.; Groh, J. H.; Gull, T. R.; Mehner, A.; Corcoran, M. F.; Damineli, A.; Hamaguchi, K. (2014). “The three-dimensional structure of the Eta Carinae Homunculus”. 《Monthly Notices of the Royal Astronomical Society》 442 (4): 3316. arXiv:1407.4096. Bibcode:2014MNRAS.442.3316S. doi:10.1093/mnras/stu1088.
- ↑ 가 나 다 라 마 바 사 아 Smith, Nathan (2006). “The Structure of the Homunculus. I. Shape and Latitude Dependence from H2and [Feii] Velocity Maps of η Carinae”. 《The Astrophysical Journal》 644 (2): 1151. arXiv:astro-ph/0602464. Bibcode:2006ApJ...644.1151S. doi:10.1086/503766.
- ↑ “Highest Resolution Image of Eta Carinae - VLT Interferometer captures raging winds in famous massive stellar system”. 《www.eso.org》. 2016년 10월 20일에 확인함.
- ↑ Gomez, H. L.; Vlahakis, C.; Stretch, C. M.; Dunne, L.; Eales, S. A.; Beelen, A.; Gomez, E. L.; Edmunds, M. G. (2010). “Submillimetre variability of Eta Carinae: Cool dust within the outer ejecta”. 《Monthly Notices of the Royal Astronomical Society: Letters》 401: L48. arXiv:0911.0176. Bibcode:2010MNRAS.401L..48G. doi:10.1111/j.1745-3933.2009.00784.x.
- ↑ Weigelt, G.; Ebersberger, J. (1986). “Eta Carinae resolved by speckle interferometry”. 《Astronomy and Astrophysics》 163: L5. Bibcode:1986A&A...163L...5W.
- ↑ Dorland, Bryan N.; Currie, Douglas G.; Hajian, Arsen R. (2004). “Did Carinae's Weigelt Blobs Originate circa 1941?”. 《The Astronomical Journal》 127 (2): 1052. Bibcode:2004AJ....127.1052D. doi:10.1086/380941.
- ↑ 가 나 Smith, Nathan (2017). “A moderately precise dynamical age for the Homunculus of Eta Carinae based on 13 years of HST imaging”. 《Monthly Notices of the Royal Astronomical Society》 471 (4): 4465–4475. arXiv:1709.06210. Bibcode:2017MNRAS.471.4465S. doi:10.1093/mnras/stx1868.
- ↑ 가 나 Davidson, Kris; Smith, Nathan; Gull, Theodore R.; Ishibashi, Kazunori; Hillier, D. J. (2001). “The Shape and Orientation of the Homunculus Nebula Based on Spectroscopic Velocities”. 《The Astronomical Journal》 121 (3): 1569. Bibcode:2001AJ....121.1569D. doi:10.1086/319419.
External links
- 3D Homunculus Nebula Astronomy Picture of the Day 2014 July 17
- Expanding Homunculus Nebula Astronomy Picture of the day (animated GIF)
- Little Homunculus and Butterfly Nebula