| 词条 | HR 178 |
| 释义 |
| name = HD 3883 }}{{Starbox observe | epoch = J2000 | ra = {{RA|00|41|36.0370}}[1] | dec = {{DEC|+24|37|44.43}}[1] | appmag_v = 6.046[3] | constell = Andromeda }}{{Starbox character | class = kA5hF1mF2[4] | b-v = 0.287[3] | variable = suspected[6] }}{{Starbox astrometry | radial_v = {{val|-15.60|0.9}}[7] | prop_mo_ra = {{val|106.272|0.499}}[1] | prop_mo_dec = {{val|-12.324|0.306}}[1] | parallax = 8.0963 | p_error = 0.2630 | parallax_footnote = [1] }}{{Starbox orbit | reference = [11] | period = 21.26 | eccentricity = 0.5 | axis = 0.126 }}{{Starbox detail | source = | component1 = | mass = | radius = 3.82[1] | luminosity = 45[1] | luminosity_bolometric = | luminosity_visual = | habitable_inner = | habitable_outer = | gravity = {{val|3.80|0.14}}[14] | temperature = {{val|7,800|200}}[14] | metal_fe = {{val|0.53|0.13}}[14] | rotation = | rotational_velocity = 18[4] | age = | age_myr = | age_gyr = }}{{Starbox catalog | names = HIP 3269, HD 3883, BD+23°94, SAO 74200. }}{{Starbox reference | Simbad = HD+3883 }}{{Starbox end}}HR 178 is a probable binary star in the constellation Andromeda. Located approximately {{convert|124|pc|ly}} distant, it is an evolved Am star[18] with a combined apparent magnitude of 6.06, meaning that it can only be seen with the naked eye on dark, clear nights. The star is suspected of variability, possibly varying between magnitudes 6.04 and 6.06.[6] The spectrum of HR 178 has been extensively studied for establishing element abundances in the evolved Am stars. It is given a spectral class of kA5hF1mF2, meaning its spectral type is A5, F1, or F2, depending on the particular spectral lines examined. The evolutionary stage of the star, and its mass determined from comparison with theoretical evolutionary tracks, is not precisely determined. However, it is very close to the end of its main sequence evolution and the margin of error in its mass is only about {{solar mass|0.1|link=y}}.[18] HR 178 has been suspected of being a binary star since 1938 when its spectrum was interpreted as being composite.[21] The pair were resolved using speckle interferometry in 1983. The companion is modelled to be between 1.5 and 3 magnitudes fainter than the primary star.[23] Although there have since been several failed attempts to resolve the pair, a tentative orbit has been calculated with a period of 21.26 years and an eccentricity of 0.5.[11] References1. ^1 2 3 4 5 6 {{cite DR2|2806529032199025536}} [2][3][4][5][6][7][8][9][10]2. ^1 {{cite journal|bibcode=1984A&AS...58..729B|title=Observations d'etoiles doubles par interferometrie des tavelures AU T2m du PIC du Midi|journal=Astronomy and Astrophysics Supplement Series|volume=58|pages=729|last1=Bonneau|first1=D.|last2=Carquillat|first2=J. M.|last3=Vidal|first3=J. L.|year=1984}} 3. ^1 {{cite journal|bibcode=1938CoPer...1...10H|title=A survey of stars with composite spectra|journal=Contributions of Perkins Observatory|volume=1|pages=10|last1=Hynek|first1=J. A.|year=1938}} 4. ^1 2 {{citation | last1=Høg | first1=E. | last2=Fabricius | first2=C. | last3=Makarov | first3=V. V. | last4=Urban | first4=S. | last5=Corbin | first5=T. | last6=Wycoff | first6=G. | last7=Bastian | first7=U. | last8=Schwekendiek | first8=P. | last9=Wicenec | first9=A. | title=The Tycho-2 catalogue of the 2.5 million brightest stars | journal=Astronomy & Astrophysics | volume=355 | pages=L27–L30 | year=2000 | bibcode=2000A&A...355L..27H | postscript=. }} 5. ^1 {{citation | title=Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system | last1=Gontcharov | first1=G. A. | journal=Astronomy Letters | volume=32 | issue=11 | pages=759–771 | date=2006 | bibcode=2006AstL...32..759G | doi=10.1134/S1063773706110065 | arxiv=1606.08053 | postscript=. }} 6. ^1 2 {{cite web|url=http://www.aavso.org/vsx/index.php?view=detail.top&oid=38882 |title=NSV 258 |author=VSX|date=18 January 2010|work=AAVSO Website|publisher=American Association of Variable Star Observers|accessdate=15 June 2013}} 7. ^1 2 {{Cite journal | doi = 10.1051/0004-6361:20040467| title = The field Am and ρ Puppis-like stars: Lithium and heavier elements| journal = Astronomy and Astrophysics| volume = 429| issue = 3| pages = 1043| year = 2005| last1 = Burkhart | first1 = C.| last2 = Coupry | first2 = M. F.| last3 = Faraggiana | first3 = R.| last4 = Gerbaldi | first4 = M.|bibcode = 2005A&A...429.1043B }} 8. ^1 2 3 {{citation | last1=Soubiran | first1=Caroline | last2=Le Campion | first2=Jean-François | last3=Brouillet | first3=Nathalie | last4=Chemin | first4=Laurent | title=The PASTEL catalogue: 2016 version | journal=Astronomy & Astrophysics | display-authors=1 | volume=591 | pages=A118 | year=2016 | bibcode=2016A&A...591A.118S | doi=10.1051/0004-6361/201628497 | arxiv=1605.07384 | postscript=. }} 9. ^1 2 {{cite journal| doi=10.1051/0004-6361/201219774| title=Dynamical masses of a selected sample of orbital binaries| journal=Astronomy & Astrophysics| volume =546| pages=5| year =2012| last1 =Malkov | first1 = O. Yu.| last2 = Tamazian | first2 =V. S.| last3 = Docobo | first3 = J. A.| last4 = Chulkov | first4 = D. A.|bibcode=2012A&A...546A..69M}} 10. ^1 2 {{cite journal|bibcode=1995ApJS...99..135A|title=The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars|journal=The Astrophysical Journal Supplement Series|volume=99|pages=135|last1=Abt|first1=Helmut A.|last2=Morrell|first2=Nidia I.|year=1995}} }}{{Stars of Andromeda}} 7 : Andromeda (constellation)|Henry Draper Catalogue objects|Am stars|HR objects|Suspected variables|Hipparcos objects|Durchmusterung objects |
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