Gliese 710

{{Short description|Star in the constellation Serpens}}

{{For|the song|Gliese 710 (song)}}

{{Starbox begin

| name = Gliese 710

}}

{{Starbox observe

| epoch = J2000

| constell = Serpens

| ra = {{RA|18|19|50.8412}}

| dec = {{DEC|-01|56|19.005}}

| appmag_v = 9.66 (9.65–9.69)

}}

{{Starbox character

| class = K7 Vk

| b-v = +1.37

| u-b = +1.26

| variable = Suspected

}}

{{Starbox astrometry

| radial_v = {{val|−14.53|0.44}}

| prop_mo_ra = {{val|-0.414|0.019}}

| prop_mo_dec = {{val|-0.108|0.017}}

| parallax = 52.3963

| p_error = 0.0171

| parallax_footnote =

| absmag_v = 8.20 (8.19–8.23)

}}

{{Starbox detail

| mass = 0.57

| radius = 0.58

| luminosity_visual = 0.045

| luminosity_bolometric = 0.091

| temperature = 4,143

| gravity = 4.66

| metal_fe = −0.11

| rotational_velocity = {{val|6.42|0.78}}

| age_myr=300

}}

{{Starbox catalog

| names=Gliese 710, BD–01°3474, HIP 89825, HD 168442, NSV 10635

}}

{{Starbox reference

| Simbad=Gl+710

| ARICNS=01481

}}

{{Starbox end}}

Gliese 710, or HIP 89825, is an orange {{solar mass|0.6|link=y}} star in the constellation Serpens Cauda. It is projected to pass near the Sun in about 1.29 million years at a predicted minimum distance of 0.051 parsecs—{{convert|0.1663|ly|AU|abbr=off|lk=on}} (about 1.6 trillion km)—about 1/25th of the current distance to Proxima Centauri. Such a distance would make for a similar brightness to the brightest planets, optimally reaching an apparent visual magnitude of about −2.7. The star's proper motion will peak around one arcminute per year, a rate of apparent motion that would be noticeable over a human lifespan. This is a timeframe, based on data from Data Release 3 from the Gaia spacecraft, well within the parameters of current models which cover the next 15 million years.

Description

Gliese 710 is currently {{Convert|62.3|ly|pc|abbr=off}} from Earth in the constellation Serpens and has a below naked-eye visual magnitude of 9.69. A stellar classification of K7 Vk means it is a small main-sequence star mostly generating energy through the thermonuclear fusion of hydrogen at its core. (The suffix 'k' indicates that the spectrum shows absorption lines from interstellar matter.) Stellar mass is about 57% of the Sun's mass with an estimated 58% of the Sun's radius. It is suspected to be a variable star that may vary in magnitude from 9.65 to 9.69. As of 2020, no planets have been detected orbiting it.

Computing and details of the closest approach

Image:Kuiper oort-en.svg and the Kuiper belt (inset)]]

In their 2010 work, Bobylev et al. suggested that Gliese 710 has an 86% chance of passing through the Oort cloud, assuming the Oort cloud to be a spheroid around the Sun with semiminor and semimajor axes of 80,000 and 100,000 AU, respectively. The distance of closest approach of Gliese 710 is generally difficult to compute precisely as it depends sensitively on its current position and velocity; Bobylev et al. estimated that Gliese 710 would pass within {{val|0.311|0.167|u=parsecs}} ({{val|1.014|0.545|u=light-years}}) of the Sun. At the time, there was even a 1-in-10,000 chance of the star penetrating into the region (d < 1,000 AU) where the influence of the passing star on Kuiper belt objects would be significant.

Results from new calculations that include input data from Gaia DR3 indicate that the flyby of Gliese 710 to the Solar System will on average be closer at {{val|0.051|0.003|u=pc}} ({{val|10635|500|fmt=commas|u=AU}}) in {{val|1.29|0.04|u=Myr}} time, but with considerably less uncertainty. The effects of such an encounter on the orbit of the Pluto–Charon system (and therefore, on the classical trans-Neptunian belt) are negligible, but Gliese 710 will traverse the outer Oort cloud (inside 100,000 AU or 0.48 pc) and reach the outskirts of the inner Oort cloud (inward of 20,000 AU).

Gliese 710 has the potential to perturb the Oort cloud in the outer Solar System, exerting enough force to send showers of comets into the inner Solar System for millions of years, triggering visibility of about ten naked-eye comets per year, and possibly causing an impact event. According to Filip Berski and Piotr Dybczyński, this event will be "the strongest disrupting encounter in the future and history of the Solar System." Earlier dynamic models indicated that the net increase in cratering rate due to the passage of Gliese 710 would be no more than 5%. They had originally estimated that the closest approach would happen in 1.36 million years when the star will approach within {{val|0.337|0.177|u=parsecs}} ({{val|1.100|0.577|u=light-years}}) of the Sun. Gaia DR2 later found the minimum perihelion distance to be {{val|0.0676|0.0157|u=parsecs}} or 13,900 ± 3,200 AU, about 1.281 million years from now.

Table of parameters of predictions of Gliese 710 encounter with Sun

class="wikitable sortable"
SourceDateEncounter distance, pcEncounter time, Myr
1999{{cvt|0.34|±|0.18|pc}}{{val|1.36|0.04}}
March 2010{{cvt|0.311|±|0.167|pc}}{{val|1.45|0.06}}
November 2016{{cvt|0.0648|±|0.0303|pc|AU}}1.35
May 2018{{cvt|0.052|±|0.01|pc|AU}}{{val|1.28|0.05}}
May 2018{{cvt|0.0676|±|0.0157|pc|AU}}1.281
December 2020{{cvt|0.051|±|0.003|pc|AU}}{{val|1.29|0.04}}
June 2022{{cvt|0.052|±|0.002|pc|AU}}{{val|1.29|0.02}}

See also

Notes

{{reflist|group=note|refs=

{{#tag:ref|From apparent magnitude and parallax: \scriptstyle M_V = m_V + 5 + 5 \log_{10} \left( \frac{\mathrm{parallax\ in\ milliarcseconds}}{1000} \right)|group="note"|name=absolute_magnitude}}

{{#tag:ref|Using the absolute visual magnitude of Gliese 710 \scriptstyle M_{V_{\ast}}=8.20 and the absolute visual magnitude of the Sun \scriptstyle M_{V_{\odot}}=4.83, the visual luminosity can be calculated by \scriptstyle \frac{L_{V_{\ast}}}{L_{V_{\odot}}}=10^{0.4\left(M_{V_{\odot}} - M_{V_{\ast}}\right)}|group="note"|name=luminosity_visual}}

}}

References

{{reflist|30em|refs=

{{cite journal|bibcode=2010MNRAS.403.1949K|title=UBV(RI)C JHK observations of Hipparcos-selected nearby stars|journal=Monthly Notices of the Royal Astronomical Society|volume=403|issue=4|pages=1949|last1=Koen|first1=C.|last2=Kilkenny|first2=D.|last3=Van Wyk|first3=F.|last4=Marang|first4=F.|year=2010|doi=10.1111/j.1365-2966.2009.16182.x|doi-access=free}}

{{cite journal | display-authors=1 |last1=Gray |first1=R. O. |first2=C. J. |last2=Corbally |first3=R. F. |last3=Garrison |first4=M. T. |last4=McFadden |first5=P. E. |last5=Robinson | title=Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I | journal=The Astronomical Journal | volume=132 | issue=1 | pages=161–170 |date=July 2006 | doi=10.1086/504637 | bibcode=2006AJ....132..161G |arxiv = astro-ph/0603770 | s2cid=119476992 }}

{{cite book | display-authors=1 |last1=Kukarkin |first1=B. V. |last2=Kholopov |first2=P. N. |last3=Pskovsky |first3=Y. P. |last4=Efremov |first4=Y. N. |last5=Kukarkina |first5=N. P. |last6=Kurochkin |first6=N. E. |last7=Medvedeva |first7=G. I. | contribution=The third edition containing information on 20437 variable stars discovered and designated till 1968 | date=1971 | title=General Catalogue of Variable Stars | edition=3rd | bibcode=1971GCVS3.C......0K }}

{{cite journal | display-authors=1 |last1=López-Santiago |first1=J. |last2=Montes |first2=D. |last3=Gálvez-Ortiz |first3=M. C. |last4=Crespo-Chacón |first4=I. |last5=Martínez-Arnáiz |first5=R. M. |last6=Fernández-Figueroa |first6=M. J. |last7=de Castro |first7=E. |last8=Cornide |first8=M. | title=A high-resolution spectroscopic survey of late-type stars: chromospheric activity, rotation, kinematics, and age | journal=Astronomy and Astrophysics | volume=514 | page=A97 |date=May 2010 | doi=10.1051/0004-6361/200913437 | bibcode=2010A&A...514A..97L |arxiv = 1002.1663 | s2cid=118640516 }}

{{cite simbad | title=GJ 710 | access-date=2019-07-06 }}

{{cite journal |last1=de la Fuente Marcos |first1=Raúl |last2=de la Fuente Marcos |first2=Carlos |name-list-style=and |year=2018 |title=An Independent Confirmation of the Future Flyby of Gliese 710 to the Solar System Using Gaia |journal=Research Notes of the AAS |volume=2 |issue=2 |pages=30 |arxiv=1805.02644 |bibcode=2018RNAAS...2...30D |doi=10.3847/2515-5172/aac2d0 |s2cid=119467738 |doi-access=free}}

{{cite journal|last1=Bailer-Jones|first1=C.A.L.

|last2=Rybizki|first2=J.

|last3=Andrae|first3=R.

|last4=Fouesnea|first4=M.

|title=New stellar encounters discovered in the second Gaia data release

|journal=Astronomy & Astrophysics

|volume=616

|pages=A37

|date=2018

|arxiv=1805.07581

|bibcode=2018A&A...616A..37B|doi=10.1051/0004-6361/201833456

|s2cid=56269929

}}

{{Cite journal |last1=Berski |first1=Filip |last2=Dybczyński |first2=Piotr A. |name-list-style=and |date=2016-11-01 |title=Gliese 710 will pass the Sun even closer |journal=Astronomy & Astrophysics |language=en |volume=595 |pages=L10 |bibcode=2016A&A...595L..10B |doi=10.1051/0004-6361/201629835 |issn=0004-6361 |doi-access=free}}

{{Cite news|title=Solar System's Next Close Encounter Will Be With Gliese 710, Say Astronomers|url=https://www.forbes.com/sites/brucedorminey/2016/12/22/solar-systems-next-close-encounter-will-be-with-gliese-710-say-astronomers/#49d76a4b993d|last=Dorminey|first=Bruce|newspaper=Forbes|access-date=2016-12-24|archive-date=2016-12-24|archive-url=https://web.archive.org/web/20161224151358/http://www.forbes.com/sites/brucedorminey/2016/12/22/solar-systems-next-close-encounter-will-be-with-gliese-710-say-astronomers/#49d76a4b993d|url-status=live}}

{{cite journal |last1=García-Sánchez |first1=Joan |last2=Preston |first2=Robert A. |last3=Jones |first3=Dayton L. |last4=Weissman |first4=Paul R. |last5=Lestrade |first5=Jean-François |last6=Latham |first6=David W. |last7=Stefanik |first7=Robert P. |display-authors=1 |date=1999 |title=Stellar encounters with the Oort cloud based on Hipparcos data |journal=The Astronomical Journal |volume=117 |issue=2 |pages=1042–1055 |bibcode=1999AJ....117.1042G |doi=10.1086/300723 |s2cid=122929693 |doi-access=free}}

{{Cite news|url=https://gizmodo.com/incoming-star-could-spawn-swarms-of-comets-when-it-pass-1790406698|title=Incoming Star Could Spawn Swarms of Comets When It Passes Our Sun|last=Dvorsky|first=George|newspaper=Gizmodo|language=en-US|access-date=2016-12-24|archive-date=2020-08-13|archive-url=https://web.archive.org/web/20200813093007/https://gizmodo.com/incoming-star-could-spawn-swarms-of-comets-when-it-pass-1790406698|url-status=live}}

{{cite journal

|last=García-Sánchez |first=J.

|author2=Weissman, P. R. |author3=Preston, R. A. |author4=Jones, D. L. |author5=Lestrade, J.-F. |author6=Latham, D. W. |author7=Stefanik, R. P. |author8= Paredes, J. M.

|title=Stellar encounters with the solar system

|journal=Astronomy and Astrophysics

|date=2001 |volume=379

|issue=2 |pages=634–659

|bibcode=2001A&A...379..634G

|doi=10.1051/0004-6361:20011330|doi-access=free }}

{{cite journal |last=Bobylev |first=Vadim V. |date=March 2010 |title=Searching for Stars Closely Encountering with the Solar System |journal=Astronomy Letters |volume=36 |issue=3 |pages=220–226 |doi=10.1134/S1063773710030060 |arxiv=1003.2160 |bibcode=2010AstL...36..220B|s2cid=118374161 }}

{{Cite Gaia DR2|4270814637616488064}}

{{cite journal |last1=de la Fuente Marcos |first1=Raúl |last2=de la Fuente Marcos |first2=Carlos |name-list-style=and |year=2020 |title=An Update on the Future Flyby of Gliese 710 to the Solar System Using Gaia EDR3: Slightly Closer and a Tad Later than Previous Estimates |journal=Research Notes of the AAS |volume=4 |issue=12 |pages=222 |arxiv= |bibcode=2020RNAAS...4..222D |doi=10.3847/2515-5172/abd18d |doi-access=free}}

{{cite journal |last1=de la Fuente Marcos |first1=Raúl |last2=de la Fuente Marcos |first2=Carlos |name-list-style=and |year=2022 |title=An Update on the Future Flyby of Gliese 710 to the Solar System Using Gaia DR3: Flyby Parameters Reproduced, Uncertainties Reduced |journal=Research Notes of the AAS |volume=6 |issue=6 |pages=136 |arxiv= |bibcode=2022RNAAS...6..136D |doi=10.3847/2515-5172/ac7b95 |doi-access=free}}

{{cite journal |bibcode=2019A&A...627A.161P |title=The CARMENES search for exoplanets around M dwarfs. Photospheric parameters of target stars from high-resolution spectroscopy. II. Simultaneous multiwavelength range modeling of activity insensitive lines |last1=Passegger |first1=V. M. |last2=Schweitzer |first2=A. |last3=Shulyak |first3=D. |last4=Nagel |first4=E. |last5=Hauschildt |first5=P. H. |last6=Reiners |first6=A. |last7=Amado |first7=P. J. |last8=Caballero |first8=J. A. |last9=Cortés-Contreras |first9=M. |last10=Domínguez-Fernández |first10=A. J. |last11=Quirrenbach |first11=A. |last12=Ribas |first12=I. |last13=Azzaro |first13=M. |last14=Anglada-Escudé |first14=G. |last15=Bauer |first15=F. F. |last16=Béjar |first16=V. J. S. |last17=Dreizler |first17=S. |last18=Guenther |first18=E. W. |last19=Henning |first19=T. |last20=Jeffers |first20=S. V. |last21=Kaminski |first21=A. |last22=Kürster |first22=M. |last23=Lafarga |first23=M. |last24=Martín |first24=E. L. |last25=Montes |first25=D. |last26=Morales |first26=J. C. |last27=Schmitt |first27=J. H. M. M. |last28=Zechmeister |first28=M. |journal=Astronomy and Astrophysics |year=2019 |volume=627 |page=627 |doi=10.1051/0004-6361/201935679 |arxiv=1907.00807 }}

{{cite journal |last1=Schweitzer |first1=Andreas |last2=Passegger |first2=V. M. |last3=Cifuentes |first3=C. |last4=Béjar |first4=Victor J. S. |last5=Cortés-Contreras |first5=M. |last6=Caballero |first6=José A. |last7=del Burgo |first7=Carlos |last8=Czesla |first8=Stefan |last9=Kürster |first9=Martin |last10=Montes |first10=David |last11=Zapatero-Osorio |first11=María Rosa |last12=Ribas |first12=Ignasi |last13=Reiners |first13=Ansgar |last14=Quirrenbach |first14=Andreas |last15=Amado |first15=Pedro J. |display-authors=1 |date=May 2019 |title=The CARMENES search for exoplanets around M dwarfs. Different roads to radii and masses of the target stars |journal=Astronomy & Astrophysics |volume=625 |pages=16 |arxiv=1904.03231 |bibcode=2019A&A...625A..68S |doi=10.1051/0004-6361/201834965 |s2cid=102351979 |id=A68 |last16=Aceituno |first16=J. |last17=Anglada-Escudé |first17=Guillem |last18=Bauer |first18=Florian F. |last19=Dreizler |first19=Stefan |last20=Jeffers |first20=Sandra V. |last21=Guenther |first21=E. W. |last22=Henning |first22=Thomas K. |last23=Kaminski |first23=Adrian |last24=Lafarga |first24=M. |last25=Marfil |first25=E. |last26=Morales |first26=Juan Carlos |last27=Schmitt |first27=Jürgen H. M. M. |last28=Seifert |first28=Walter |last29=Solano |first29=E. |last30=Tabernero |first30=H. M. |last31=Zechmeister |first31=Mathias}}

{{cite journal |bibcode=2012AstL...38..331A |title=XHIP: An extended hipparcos compilation |last1=Anderson |first1=E. |last2=Francis |first2=Ch. |journal=Astronomy Letters |date=2012 |volume=38 |issue=5 |page=331 |doi=10.1134/S1063773712050015 |arxiv=1108.4971 }}

}}