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| caption = V488 Persei (blue star in the middle) with the ] |
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The disk was first found with ] and ] data. The researchers find dust with a temperature of about 800 ] (K) at 0.06 ] (AU). The researchers suspect that two planetary embroys collided with each other at distances similar to transiting ], known at the time. At first it was suspected that the disk also contains a cold component at 120 K.<ref name="Zuckerman2012" /> Using ] observations it was indeed found that the disk has a cold component with a temperature of around 130 K.<ref name="Sankar2021"/> There are currently two interpretations of the disk. One work interprets the ] as two rings: an inner ring at 0.30–0.35 AU and an outer ring at 25–45 AU.<ref name="Rieke2021" /> Another work interprets the excess as two disks: an inner disk at around 0.07 AU and an outer disk at 2.7 AU.<ref name="Sankar2021" /> |
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The disk was first found with ] and ] data. The researchers find dust with a temperature of about 800 ] (K) at 0.06 ] (AU). The researchers suspect that two planetary embroys collided with each other at distances similar to transiting ], known at the time. At first it was suspected that the disk also contains a cold component at 120 K.<ref name="Zuckerman2012" /> Using ] observations it was indeed found that the disk has a cold component with a temperature of around 130 K.<ref name="Sankar2021"/> There are currently two interpretations of the disk. One work interprets the ] as two rings: an inner ring at 0.30–0.35 AU and an outer ring at 25–45 AU.<ref name="Rieke2021" /> Another work interprets the excess as two disks: an inner disk at around 0.07 AU and an outer disk at 2.7 AU.<ref name="Sankar2021" /> |
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In 2021 it was found that the infrared brightness of the system is extreme variable, similar to ]. This was found from a observation campaign with Spitzer. This work found that one major event occured in 2019, leading to an increase of infrared brightness. This event was produced by the collision of two objects 60 km in size. The disk was however extreme before this event and variable over a period of 15 years, meaning additional collisions must take place in the disk. The same work suggests that the members of a belt at 0.3 AU, similar to the ], are perturbed by a ] or ]. This results in a high level of collisions between planetesimals and the dust will be dragged towards the star due to the ]. Because the dust is removed very fast a high level of collisions must be present in the inner region. The system might be an analogue to the ] in the ].<ref name="Rieke2021" /> One work failed to detect ] emission in the mid-infrared with ]/COMICS. The researchers interpret this as dust grains composed primarily of ]. It could be interpreted as a similar scenario to the formation of planet ]. In this scenario a rocky planet is subjected to erosive bombardment and the ejecta from the interior of the planet is ground into small particles. This scenario is more likely with an inner system packed with ]-type and ]-type planets.<ref name="Sankar2021" /> |
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In 2021 it was found that the infrared brightness of the system is extreme variable, similar to ]. This was found from a observation campaign with Spitzer. This work found that one major event occured in 2019, leading to an increase of infrared brightness. This event was produced by the collision of two objects 60 km in size. The disk was however extreme before this event and variable over a period of 15 years, meaning additional collisions must take place in the disk. The same work suggests that the objects in an ] at 0.3 AU are perturbed by a ] or ]. This results in a high level of collisions between planetesimals and the dust will be dragged towards the star due to the ]. A high level of collisions are happening in the inner region, because the dust is removed very fast. The system might be an analogue to the ] in the ].<ref name="Rieke2021" /> Another work failed to detect ] emission in the mid-infrared with ]/COMICS. The researchers interpret this as dust grains composed primarily of ]. The researchers interpret this observation as a similar scenario that formed planet ]. In this scenario a rocky planet is subjected to erosive bombardment and the ejecta from the interior of the planet is ground into small particles. This scenario is more likely with an inner system packed with ]-type and ]-type planets.<ref name="Sankar2021" /> |
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== See also == |
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* ] |
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== References == |
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== References == |
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{{reflist|refs= |
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<ref name="Sankar2021">{{Cite journal |last=Sankar |first=Swetha |last2=Melis |first2=Carl |last3=Klein |first3=Beth L. |last4=Fulton |first4=B. J. |last5=Zuckerman |first5=B. |last6=Song |first6=Inseok |last7=Howard |first7=Andrew W. |date=2021-11-01 |title=V488 Per Revisited: No Strong Mid-infrared Emission Features and No Evidence for Stellar/substellar Companions |url=https://ui.adsabs.harvard.edu/abs/2021ApJ...922...75S/abstract |journal=The Astrophysical Journal |volume=922 |pages=75 |arxiv=2108.03700 |bibcode=2021ApJ...922...75S |doi=10.3847/1538-4357/ac19a8 |issn=0004-637X}}</ref> |
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<ref name="Sankar2021">{{Cite journal |last1=Sankar |first1=Swetha |last2=Melis |first2=Carl |last3=Klein |first3=Beth L. |last4=Fulton |first4=B. J. |last5=Zuckerman |first5=B. |last6=Song |first6=Inseok |last7=Howard |first7=Andrew W. |date=2021-11-01 |title=V488 Per Revisited: No Strong Mid-infrared Emission Features and No Evidence for Stellar/substellar Companions |journal=The Astrophysical Journal |volume=922 |issue=1 |pages=75 |arxiv=2108.03700 |bibcode=2021ApJ...922...75S |doi=10.3847/1538-4357/ac19a8 |doi-access=free |issn=0004-637X}}</ref> |
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<ref name="Zuckerman2015">{{Cite journal |last=Zuckerman |first=B. |date=2015-01-01 |title=Warm Dusty Debris Disks and Distant Companion Stars: V488 Per and 2M1337 |url=https://ui.adsabs.harvard.edu/abs/2015ApJ...798...86Z/abstract |journal=The Astrophysical Journal |volume=798 |pages=86 |arxiv=1411.2197 |bibcode=2015ApJ...798...86Z |doi=10.1088/0004-637X/798/2/86 |issn=0004-637X}}</ref> |
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<ref name="Zuckerman2015">{{Cite journal |last=Zuckerman |first=B. |date=2015-01-01 |title=Warm Dusty Debris Disks and Distant Companion Stars: V488 Per and 2M1337 |url=https://ui.adsabs.harvard.edu/abs/2015ApJ...798...86Z/abstract |journal=The Astrophysical Journal |volume=798 |issue=2 |pages=86 |arxiv=1411.2197 |bibcode=2015ApJ...798...86Z |doi=10.1088/0004-637X/798/2/86 |issn=0004-637X}}</ref> |
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<ref name="Zuckerman2012">{{Cite journal |last=Zuckerman |first=B. |last2=Melis |first2=Carl |last3=Rhee |first3=Joseph H. |last4=Schneider |first4=Adam |last5=Song |first5=Inseok |date=2012-05-25 |title=Stellar Membership and Dusty Debris Disks in the α Persei Cluster |url=https://iopscience.iop.org/article/10.1088/0004-637X/752/1/58 |journal=The Astrophysical Journal |volume=752 |issue=1 |pages=58 |arxiv=1204.3950 |bibcode=2012ApJ...752...58Z |doi=10.1088/0004-637x/752/1/58 |issn=0004-637X}}</ref> |
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<ref name="Zuckerman2012">{{Cite journal |last1=Zuckerman |first1=B. |last2=Melis |first2=Carl |last3=Rhee |first3=Joseph H. |last4=Schneider |first4=Adam |last5=Song |first5=Inseok |date=2012-05-25 |title=Stellar Membership and Dusty Debris Disks in the α Persei Cluster |url=https://iopscience.iop.org/article/10.1088/0004-637X/752/1/58 |journal=The Astrophysical Journal |volume=752 |issue=1 |pages=58 |arxiv=1204.3950 |bibcode=2012ApJ...752...58Z |doi=10.1088/0004-637x/752/1/58 |issn=0004-637X}}</ref> |
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<ref name="Rieke2021">{{Cite journal |last=Rieke |first=G. H. |last2=Su |first2=K. Y. L. |last3=Melis |first3=Carl |last4=Gáspár |first4=András |date=2021-09-01 |title=Extreme Variability of the V488 Persei Debris Disk |url=https://ui.adsabs.harvard.edu/abs/2021ApJ...918...71R/abstract |journal=The Astrophysical Journal |volume=918 |pages=71 |arxiv=2108.02901 |bibcode=2021ApJ...918...71R |doi=10.3847/1538-4357/ac0dc4 |issn=0004-637X}}</ref> |
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<ref name="Rieke2021">{{Cite journal |last1=Rieke |first1=G. H. |last2=Su |first2=K. Y. L. |last3=Melis |first3=Carl |last4=Gáspár |first4=András |date=2021-09-01 |title=Extreme Variability of the V488 Persei Debris Disk |journal=The Astrophysical Journal |volume=918 |issue=2 |pages=71 |arxiv=2108.02901 |bibcode=2021ApJ...918...71R |doi=10.3847/1538-4357/ac0dc4 |doi-access=free |issn=0004-637X}}</ref> |
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<ref name="Stauffer1985">{{Cite journal |last=Stauffer |first=J. R. |last2=Hartmann |first2=L. W. |last3=Burnham |first3=J. N. |last4=Jones |first4=B. F. |date=February 1985 |title=Evolution of low-mass stars in the alpha Persei cluster. |url=https://ui.adsabs.harvard.edu/abs/1985ApJ...289..247S/abstract |journal=Astrophysical Journal |volume=289 |pages=247-261 |bibcode=1985ApJ...289..247S |doi=10.1086/162885}}</ref> |
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<ref name="Stauffer1985">{{Cite journal |last1=Stauffer |first1=J. R. |last2=Hartmann |first2=L. W. |last3=Burnham |first3=J. N. |last4=Jones |first4=B. F. |date=February 1985 |title=Evolution of low-mass stars in the alpha Persei cluster. |url=https://ui.adsabs.harvard.edu/abs/1985ApJ...289..247S/abstract |journal=Astrophysical Journal |volume=289 |pages=247–261 |bibcode=1985ApJ...289..247S |doi=10.1086/162885}}</ref> |
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<ref name="Moór2021">{{Cite journal |last=Moór |first=Attila |last2=Ábrahám |first2=Péter |last3=Szabó |first3=Gyula |last4=Vida |first4=Krisztián |last5=Cataldi |first5=Gianni |last6=Derekas |first6=Alíz |last7=Henning |first7=Thomas |last8=Kinemuchi |first8=Karen |last9=Kóspál |first9=Ágnes |last10=Kovács |first10=József |last11=Pál |first11=András |last12=Sarkis |first12=Paula |last13=Seli |first13=Bálint |last14=Szabó |first14=Zsófia M. |last15=Takáts |first15=Katalin |date=2021-03-01 |title=A New Sample of Warm Extreme Debris Disks from the ALLWISE Catalog |url=https://ui.adsabs.harvard.edu/abs/2021ApJ...910...27M/abstract |journal=The Astrophysical Journal |volume=910 |pages=27 |arxiv=2103.00568 |bibcode=2021ApJ...910...27M |doi=10.3847/1538-4357/abdc26 |issn=0004-637X}}</ref> |
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<ref name="Moór2021">{{Cite journal |last1=Moór |first1=Attila |last2=Ábrahám |first2=Péter |last3=Szabó |first3=Gyula |last4=Vida |first4=Krisztián |last5=Cataldi |first5=Gianni |last6=Derekas |first6=Alíz |last7=Henning |first7=Thomas |last8=Kinemuchi |first8=Karen |last9=Kóspál |first9=Ágnes |last10=Kovács |first10=József |last11=Pál |first11=András |last12=Sarkis |first12=Paula |last13=Seli |first13=Bálint |last14=Szabó |first14=Zsófia M. |last15=Takáts |first15=Katalin |date=2021-03-01 |title=A New Sample of Warm Extreme Debris Disks from the ALLWISE Catalog |journal=The Astrophysical Journal |volume=910 |issue=1 |pages=27 |arxiv=2103.00568 |bibcode=2021ApJ...910...27M |doi=10.3847/1538-4357/abdc26 |doi-access=free |issn=0004-637X}}</ref> |
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<ref name="GaiaDR3">{{Cite Gaia DR3|249236647249997696}}</ref> |
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<ref name="GaiaDR3">{{Cite Gaia DR3|249236647249997696}}</ref> |
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{{Perseus (constellation)}} |
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Candidate wide companions around V488 Persei were identified in 2015. Another work does point out problems with this approach, pointing out that wide companions cannot be distinguished from unrelated cluster members.
In 2021 it was found that the infrared brightness of the system is extreme variable, similar to NGC 2547-ID8. This was found from a observation campaign with Spitzer. This work found that one major event occured in 2019, leading to an increase of infrared brightness. This event was produced by the collision of two objects 60 km in size. The disk was however extreme before this event and variable over a period of 15 years, meaning additional collisions must take place in the disk. The same work suggests that the objects in an asteroid-like belt at 0.3 AU are perturbed by a giant planet or brown dwarf. This results in a high level of collisions between planetesimals and the dust will be dragged towards the star due to the stellar wind. A high level of collisions are happening in the inner region, because the dust is removed very fast. The system might be an analogue to the late heavy bombardment in the solar system. Another work failed to detect silicate emission in the mid-infrared with Subaru/COMICS. The researchers interpret this as dust grains composed primarily of metallic iron. The researchers interpret this observation as a similar scenario that formed planet Mercury. In this scenario a rocky planet is subjected to erosive bombardment and the ejecta from the interior of the planet is ground into small particles. This scenario is more likely with an inner system packed with earth-type and super-earth-type planets.
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