14 Lacertae

{{Starbox begin

| name = 14 Lacertae

}}

{{Starbox image

| image = 250px

| caption = A visual band light curve for V360 Lacertae, adapted from Linnell et al. (2006)

}}

{{Starbox observe

| epoch = J2000

| constell = Lacerta

| ra = {{RA|22|50|21.77721}}

| dec = {{DEC|+41|57|12.1795}}

| appmag_v = 5.91

}}

{{Starbox character

| type =

| class = B3IV:eaV {{nowrap|(B4 + F9 III)}}

| b-v = +0.083

| u-b = −0.508

| variable = β Lyr

}}

{{Starbox astrometry

| radial_v = {{Val|−15.8|3.1}}

| prop_mo_ra = +6.047

| prop_mo_dec = +1.124

| parallax = 2.0147

| p_error = 0.1990

| parallax_footnote =

| absmag_v =

}}

{{Starbox orbit

| reference =

| period_unitless = {{Val|10.085415|0.000080|u=days}}

| axis =

| axis_unitless =

| eccentricity = 0.0

| inclination =

| node =

| periastron = {{Val|2441170.285|0.029}}

| periarg =

| k1 = {{Val|25.8|1.7}}

| k2 = {{Val|159.2|0.2}}

}}

{{Starbox detail

| source =

| component1 = 14 Lac A

| mass = {{Val|7.45|0.3}}

| radius = (polar) 7.55

| luminosity =

| temperature = (Polar) {{Val|18000|1000|fmt=commas}}

| gravity = 3.55

| metal_fe =

| rotational_velocity =

| age_myr =

| component2 = 14 Lac B

| mass2 = {{Val|1.21|0.05}}

| radius2 = (polar) 8.85

| temperature2 = (polar) {{Val|6000|200|fmt=commas}}

| gravity2 = 2.65

}}

{{Starbox catalog

| names = {{odlist | V=V360 Lac | F=14 Lac | BD=+41°4623 | FK5= | HD=216200 | HIP=112778 | HR=8690 | SAO=52412 | WDS=J22504+4157 }}

}}

{{Starbox reference

| Simbad = 14+Lac

}}

14 Lacertae is a binary star system in the northern constellation Lacerta, located around 1,600 light years away. It has the variable star designation V360 Lacertae; 14 Lacertae is the Flamsteed designation. The system is barely visible to the naked eye in good seeing conditions, having a peak apparent visual magnitude of 5.91. It is moving closer to the Earth with a heliocentric radial velocity of −16 km/s.

This is a double-lined spectroscopic binary in a close, circular orbit with a period of 10.08 days and a separation of {{Convert|40.327|solar radius|Gm|abbr=on|lk=on}}. The orbital inclination is {{Val|65|1|u=°}}. 14 Lac is a variable star system that, once per orbit, shows a primary minimum with a 0.07 magnitude decrease and a secondary minimum with a decrease of 0.02. The primary component is a Be star that is spinning rapidly at its critical velocity. The lower mass secondary is synchronously rotating and is filling its Roche lobe. The rapid rotation of the primary may have been caused by mass transfer from the secondary.

Samus et al. (2017) classify this as a detached Beta Lyrae-type eclipsing binary, although they note there is some uncertainty in the classification. Bossi et al. (1998) argued that the system is neither an eclipsing binary nor an ellipsoidal variable. Instead they propose the variability is caused by distortion of a gaseous shell by the secondary component. Linnell et al. (2006) demonstrated that the light curve is mostly caused by tidal distortion in combination with illumination of the lower mass secondary by the primary.

References

{{reflist|refs=

{{citation

| title=Properties and nature of Be stars. 24. Better data and model for the Be+F binary V360 Lacertae

| display-authors=1 | last1=Linnell | first1=A. P. | author1-link=Albert Paul Linnell

| last2=Harmanec | first2=P. | last3=Koubský | first3=P.

| last4=Božić | first4=H. | last5=Yang | first5=S.

| last6=Ruždjak | first6=D. | last7=Sudar | first7=D.

| last8=Libich | first8=J. | last9=Eenens | first9=P.

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| doi=10.1051/0004-6361:20053792 | bibcode=2006A&A...455.1037L | doi-access=free }}

{{citation

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| display-authors=1 | journal=Astronomy and Astrophysics

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{{citation

| title=Properties and nature of Be stars. 17. V360 Lac = HD 216200 is a B3e + F9IV: binary

| display-authors=1 | last1=Hill | first1=G.

| last2=Harmanec | first2=P. | last3=Pavlovski | first3=K.

| last4=Bozic | first4=H. | last5=Hadrava | first5=P.

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| journal=Astronomy and Astrophysics

| volume=324 | pages=965–976 | date=August 1997

| bibcode=1997A&A...324..965H | postscript=. }}

{{citation

| title=14 Lacertae: A case of shell-orbit coupling?

| display-authors=1 | last1=Bossi | first1=M.

| last2=Nunez | first2=N. S. | last3=Guerrero | first3=G.

| last4=Sareyan | first4=J. -P. | last5=Alvarez | first5=M.

| journal=Astronomy and Astrophysics Supplement

| volume=127 | pages=433–444 | date=February 1998

| issue=3 | doi=10.1051/aas:1998112 | bibcode=1998A&AS..127..433B | doi-access=free }}

{{citation

| title=Properties and nature of Be stars. 30. Reliable physical properties of a semi-detached B9.5e+G8III binary BR CMi = HD 61273 compared to those of other well studied semi-detached emission-line binaries

| last1=Harmanec | first1=P. | last2=Koubský | first2=P.

| last3=Nemravová | first3=J. A. | last4=Royer | first4=F.

| last5=Briot | first5=D. | last6=North | first6=P.

| last7=Lampens | first7=P. | last8=Frémat | first8=Y.

| last9=Yang | first9=S. | last10=Božić | first10=H.

| last11=Kotková | first11=L. | last12=Škoda | first12=P.

| last13=Šlechta | first13=M. | last14=Korčáková | first14=D.

| last15=Wolf | first15=M. | last16=Zasche | first16=P.

| journal=Astronomy & Astrophysics | display-authors=1 | postscript=.

| volume=573 | id=A107 | pages=17 | date=January 2015

| doi=10.1051/0004-6361/201424640 | arxiv=1411.5651 | bibcode=2015A&A...573A.107H | doi-access=free }}

{{citation