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Star formation
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Star formation
Object classes
Interstellar medium
Molecular cloud
Bok globule
Dark nebula
Young stellar object
Protostar
T Tauri star
Pre-main-sequence star
Herbig Ae/Be star
Herbig–Haro object
Theoretical concepts
Accretion
Initial mass function
Jeans instability
Kelvin–Helmholtz mechanism
Nebular hypothesis
Planetary migration
Star portal
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Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as "stellar nurseries" or "star-forming regions", collapse and form stars.[1] As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.
Contents
[hide]
1 Stellar nurseries
1.1 Interstellar clouds
1.2 Cloud collapse
2 Protostar
3 Observations
3.1 Notable pathfinder objects
4 Low mass and high mass star formation
5 See also
6 References
Stellar nurseries[edit]
Hubble telescope image known as Pillars of Creation, where stars are forming in the Eagle Nebula.
Interstellar clouds[edit]
A spiral galaxy like the Milky Way contains stars, stellar remnants, and a diffuse interstellar medium (ISM) of gas and dust. The interstellar medium consists of 10−4 to 106 particles per cm3 and is typically composed of roughly 70% hydrogen by mass, with most of the remaining gas consisting of helium. This medium has been chemically enriched by trace amounts of heavier elements that were ejected from stars as they passed beyond the end of their main sequence lifetime. Higher density regions of the interstellar medium form clouds, or diffuse nebulae,[2] where star formation takes place.[3] In contrast to spirals, an elliptical galaxy loses the cold component of its interstellar medium within roughly a billion years, which hinders the galaxy from forming diffuse nebulae except through mergers with other galaxies.[4]
In the dense nebulae where stars are produced, much of the hydrogen is in the molecular (H2) form, so these nebulae are called molecular clouds.[3] Observations indicate that the coldest clouds tend to form low-mass stars, observed first in the infrared inside the clouds, then in visible light at their surface when the clouds dissipate, while giant molecular clouds, which are generally warmer, produce stars of all masses.[5] These giant molecular clouds have typical densities of 100 particles per cm3, diameters of 100 light-years (9.5×1014 km), masses of up to 6 million solar masses (M☉),[6] and an average interior temperature of 10 K. About half the total mass of the galactic ISM is found in molecular clouds[7] and in the Milky Way there are an estimated 6,000 molecular clouds, each with more than 100,000 M☉.[8] The nearest nebula to the Sun where massive stars are being formed is the Orion nebula, 1,300 ly (1.2×1016 km) away.[9] However, lower mass star formation is occurring about 400–450 light years distant in the ρ Ophiuchi cloud complex.[10]
A more compact site of star formation is the opaque clouds of dense gas and dust known as Bok globules; so named after the astronomer Bart Bok. These can form in association with collapsing molecular clouds or possibly independently.[11] The Bok globules are typically up to a light year across and contain a few solar masses.[12] They can be observed as dark clouds silhouetted against bright emission nebulae or background stars. Over half the known Bok globules have been found to contain newly forming stars.[13]
Assembly of galaxy in early Universe.[14]
Cloud collapse[edit]
An interstellar cloud of gas will remain in hydrostatic equilibrium as long as the kinetic energy of the gas pressure is in balance with the potential energy of the internal gravitational force. Mathematically this is expressed using the virial theorem, which states that, to maintain equilibrium, the gravitational potential energy must equal twice the internal thermal energy.[15] If a cloud is massive enough that the gas pressure is insufficient to support it, the cloud will undergo gravitational collapse. The mass above which a cloud will undergo such collapse is called the Jeans mass. The Jeans mass depends on the temperature and density of the cloud, but is typically thousands to tens of thousands of solar masses.[3] This coincides with the typical mass of an open cluster of stars, which is the end product of a collapsing cloud.[16]
ALMA observations of the Orion Nebula complex provide insights into explosions at star birth.[17]
In triggered star formation, one of several events might occur to compress a molecular cloud and initiate its gravitational collapse. Molecular clouds may collide with each other, or a nearby supernova explosion can be a trigger, sending shocked matter into the cloud at very high speeds.[3] (The resulting new stars may themselves soon produce supernovae, producing self-propagating star formation.) Alternatively, galactic collisions can trigger massive starbursts of star formation as the gas clouds in each galaxy are compressed and agitated by tidal forces.[18] The latter mechanism may be responsible for the formation of globular clusters.[19]
A supermassive black hole at the core of a galaxy may serve to regulate the rate of star formation in a galactic nucleus. A black hole that is accreting infalling matter can become active, emitting a strong wind through a collimated relativistic jet. This can limit further star formation. Massive black holes ejecting radio-frequency-emitting particles at near-light speed can also block the formation of new stars in aging galaxies.[20] However, the radio emissions around the jets may also trigger star formation. Likewise, a weaker jet may trigger star formation when it collides with a cloud.[21]
Dwarf galaxy ESO 553-46 has one of the highest rates of star formation of the 1000 or so galaxies nearest to the Milky Way.[22]
As it collapses, a molecular cloud breaks into smaller and smaller pieces in a hierarchical manner, until the fragments reach stellar mass. In each of these fragments, the collapsing gas radiates away the energy gained by the release of gravitational potential energy. As the density increases, the fragments become opaque and are thus less efficient at radiating away their energy. This raises the temperature of the cloud and inhibits further fragmentation. The fragments now condense into rotating spheres of gas that serve as stellar embryos.[23]
Complicating this picture of a collapsing cloud are the effects of turbulence, macroscopic flows, rotation, magnetic fields and the cloud geometry. Both rotation and magnetic fields can hinder the collapse of a cloud.[24][25] Turbulence is instrumental in causing fragmentation of the cloud, and on the smallest scales it promotes collapse.[26]
Protostar[edit]
Main article: Protostar
LH 95 stellar nursery in Large Magellanic Cloud.
A protostellar cloud will continue to collapse as long as the gravitational binding energy can be eliminated. This excess energy is primarily lost through radiation. However, the collapsing cloud will eventually become opaque to its own radiation, and the energy must be removed through some other means. The dust within the cloud becomes heated to temperatures of 60–100 K, and these particles radiate at wavelengths in the far infrared where the cloud is transparent. Thus the dust mediates the further collapse of the cloud.[27]
During the collapse, the density of the cloud increases towards the center and thus the middle region becomes optically opaque first. This occurs when the density is about 10−13 g / cm3. A core region, called the First Hydrostatic Core, forms where the collapse is essentially halted. It continues to increase in temperature as determined by the virial theorem. The gas falling toward this opaque region collides with it and creates shock waves that further heat the core.[28]
Composite image showing young stars in and around molecular cloud Cepheus B.
When the core temperature reaches about 2000 K, the thermal energy dissociates the H2 molecules.[28] This is followed by the ionization of the hydrogen and helium atoms. These processes absorb the energy of the contraction, allowing it to continue on timescales comparable to the period of collapse at free fall velocities.[29] After the density of infalling material has reached about 10−8 g / cm3, that material is sufficiently transparent to allow energy radiated by the protostar to escape. The combination of convection within the protostar and radiation from its exterior allow the star to contract further.[28] This continues until the gas is hot enough for the internal pressure to support the protostar against further gravitational collapse—a state called hydrostatic equilibrium. When this accretion phase is nearly complete, the resulting object is known as a protostar.[3]
N11, part of a complex network of gas clouds and star clusters within our neighbouring galaxy, the Large Magellanic Cloud.
Accretion of material onto the protostar continues partially from the newly formed circumstellar disc. When the density and temperature are high enough, deuterium fusion begins, and the outward pressure of the resultant radiation slows (but does not stop) the collapse. Material comprising the cloud continues to "rain" onto the protostar. In this stage bipolar jets are produced called Herbig-Haro objects. This is probably the means by which excess angular momentum of the infalling material is expelled, allowing the star to continue to form.
Star formation region Lupus 3.[30]
When the surrounding gas and dust envelope disperses and accretion process stops, the star is considered a pre–main sequence star (PMS star). The energy source of these objects is gravitational contraction, as opposed to hydrogen burning in main sequence stars. The PMS star follows a Hayashi track on the Hertzsprung–Russell (H–R) diagram.[31] The contraction will proceed until the Hayashi limit is reached, and thereafter contraction will continue on a Kelvin–Helmholtz timescale with the temperature remaining stable. Stars with less than 0.5 M☉ thereafter join the main sequence. For more massive PMS stars, at the end of the Hayashi track they will slowly collapse in near hydrostatic equilibrium, following the Henyey track.[32]
Finally, hydrogen begins to fuse in the core of the star, and the rest of the enveloping material is cleared away. This ends the protostellar phase and begins the star's main sequence phase on the H–R diagram.
The stages of the process are well defined in stars with masses around 1 M☉ or less. In high mass stars, the length of the star formation process is comparable to the other timescales of their evolution, much shorter, and the process is not so well defined. The later evolution of stars are studied in stellar evolution.
Protostar
Protostar outburst - HOPS 383 (2015).
Observations[edit]
The Orion Nebula is an archetypical example of star formation, from the massive, young stars that are shaping the nebula to the pillars of dense gas that may be the homes of budding stars.
Key elements of star formation are only available by observing in wavelengths other than the optical. The protostellar stage of stellar existence is almost invariably hidden away deep inside dense clouds of gas and dust left over from the GMC. Often, these star-forming cocoons known as Bok globules, can be seen in silhouette against bright emission from surrounding gas.[33] Early stages of a star's life can be seen in infrared light, which penetrates the dust more easily than visible light.[34] Observations from the Wide-field Infrared Survey Explorer (WISE) have thus been especially important for unveiling numerous Galactic protostars and their parent star clusters.[35][36] Examples of such embedded star clusters are FSR 1184, FSR 1190, Camargo 14, Camargo 74, Majaess 64, and Majaess 98.[37]
Star-forming region S106.
The structure of the molecular cloud and the effects of the protostar can be observed in near-IR extinction maps (where the number of stars are counted per unit area and compared to a nearby zero extinction area of sky), continuum dust emission and rotational transitions of CO and other molecules; these last two are observed in the millimeter and submillimeter range. The radiation from the protostar and early star has to be observed in infrared astronomy wavelengths, as the extinction caused by the rest of the cloud in which the star is forming is usually too big to allow us to observe it in the visual part of the spectrum. This presents considerable difficulties as the Earth's atmosphere is almost entirely opaque from 20μm to 850μm, with narrow windows at 200μm and 450μm. Even outside this range, atmospheric subtraction techniques must be used.
Young stars (purple) revealed by X-ray inside the NGC 2024 star-forming region.[38]
X-ray observations have proven useful for studying young stars, since X-ray emission from these objects is 100–100,000 times stronger than X-ray emission from main-sequence stars.[39] The earliest detections of X-rays from T Tauri stars were made by the Einstein X-ray Observatory.[40][41] For low-mass stars X-rays are generated by the heating of the stellar corona through magnetic reconnection, while for high-mass O and early B-type stars X-rays are generated through supersonic shocks in the stellar winds. Photons in the soft X-ray energy range covered by the Chandra X-ray Observatory and XMM Newton may penetrate the interstellar medium with only moderate absorption due to gas, making the X-ray a useful wavelength for seeing the stellar populations within molecular clouds. X-ray emission as evidence of stellar youth makes this band particularly useful for performing censuses of stars in star-forming regions, given that not all young stars have infrared excesses.[42] X-ray observations have provided near-complete censuses of all stellar-mass objects in the Orion Nebula Cluster and Taurus Molecular Cloud.[43][44]
The formation of individual stars can only be directly observed in the Milky Way Galaxy, but in distant galaxies star formation has been detected through its unique spectral signature.
Initial research indicates star-forming clumps start as giant, dense areas in turbulent gas-rich matter in young galaxies, live about 500 million years, and may migrate to the center of a galaxy, creating the central bulge of a galaxy.[45]
On February 21, 2014, NASA announced a greatly upgraded database for tracking polycyclic aromatic hydrocarbons (PAHs) in the universe. According to scientists, more than 20% of the carbon in the universe may be associated with PAHs, possible starting materials for the formation of life. PAHs seem to have been formed shortly after the Big Bang, are widespread throughout the universe, and are associated with new stars and exoplanets.[46]
In February 2018, astronomers reported, for the first time, a signal of the reionization epoch, an indirect detection of light from the earliest stars formed - about 180 million years after the Big Bang.[47]
Notable pathfinder objects[edit]
MWC 349 was first discovered in 1978, and is estimated to be only 1,000 years old.
VLA 1623 – The first exemplar Class 0 protostar, a type of embedded protostar that has yet to accrete the majority of its mass. Found in 1993, is possibly younger than 10,000 years.[48]
L1014 – An extremely faint embedded object representative of a new class of sources that are only now being detected with the newest telescopes. Their status is still undetermined, they could be the youngest low-mass Class 0 protostars yet seen or even very low-mass evolved objects (like a brown dwarf or even an interstellar planet).[49]
IRS 8* – The youngest known main sequence star in the Galactic Center region, discovered in August 2006. It is estimated to be 3.5 million years old.[50]
Low mass and high mass star formation[edit]
Star-forming region Westerhout 40 and the Serpens-Aquila Rift- cloud filaments containing new stars fill the region.[51][52]
Stars of different masses are thought to form by slightly different mechanisms. The theory of low-mass star formation, which is well-supported by a plethora of observations, suggests that low-mass stars form by the gravitational collapse of rotating density enhancements within molecular clouds. As described above, the collapse of a rotating cloud of gas and dust leads to the formation of an accretion disk through which matter is channeled onto a central protostar. For stars with masses higher than about 8 M☉, however, the mechanism of star formation is not well understood.
Massive stars emit copious quantities of radiation which pushes against infalling material. In the past, it was thought that this radiation pressure might be substantial enough to halt accretion onto the massive protostar and prevent the formation of stars with masses more than a few tens of solar masses.[53] Recent theoretical work has shown that the production of a jet and outflow clears a cavity through which much of the radiation from a massive protostar can escape without hindering accretion through the disk and onto the protostar.[54][55] Present thinking is that massive stars may therefore be able to form by a mechanism similar to that by which low mass stars form.
There is mounting evidence that at least some massive protostars are indeed surrounded by accretion disks. Several other theories of massive star formation remain to be tested observationally. Of these, perhaps the most prominent is the theory of competitive accretion, which suggests that massive protostars are "seeded" by low-mass protostars which compete with other protostars to draw in matter from the entire parent molecular cloud, instead of simply from a small local region.[56][57]
Another theory of massive star formation suggests that massive stars may form by the coalescence of two or more stars of lower mass.[58]
See also[edit]
Accretion
Champagne flow model
Chronology of the universe
Formation and evolution of the Solar System
Galaxy formation and evolution
List of star-forming regions in the Local Group
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Jump up ^ I. A. Bonnell; M. R. Bate; H. Zinnecker (1998). "On the formation of massive stars". Monthly Notices of the Royal Astronomical Society. 298 (1): 93–102. arXiv:astro-ph/9802332  . Bibcode:1998MNRAS.298...93B. doi:10.1046/j.1365-8711.1998.01590.x.
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The Man Who Invented Christmas (film)
From Wikipedia, the free encyclopedia
Jump to: navigation, search
The Man Who Invented Christmas
Theatrical release poster
Directed by
Bharat Nalluri
Produced by
Robert Mickelson
Ian Sharples
Paula Mazur
Mitchell Kaplan
Andrew Karpen
Vadim Jean
Written by
Susan Coyne
Based on
The Man Who Invented Christmas
by Les Standiford
Starring
Dan Stevens
Christopher Plummer
Jonathan Pryce
Music by
Mychael Danna
Cinematography
Ben Smithard
Edited by
Stephen O'Connell
Jamie Pearson
Production
company
Parallel Films
Rhombus Media
Distributed by
Elevation Pictures (Canada)
Wildcard Distribution (Ireland)
Release date
10 November 2017 (2017-11-10) (Cork Film Festival[1])
22 November 2017 (2017-11-22) (Canada)
Running time
104 minutes[2]
Country
Ireland
Canada
Language
English
Box office
$8.1 million[3]
The Man Who Invented Christmas is a 2017 biographical drama film directed by Bharat Nalluri and written by Susan Coyne based on the book of the same name by Les Standiford. It stars Dan Stevens, Christopher Plummer, and Jonathan Pryce. The plot follows Charles Dickens (Stevens) at the time when he wrote A Christmas Carol, and how Dickens's fictional character Ebenezer Scrooge (Plummer) was influenced by his real-life father, John Dickens (Pryce).
It was released by Bleecker Street in the United States on November 22, 2017[4] and in the United Kingdom on December 1, 2017.[5]
Contents
[hide]
1 Synopsis
2 Cast
3 Release
3.1 Critical response
3.2 Accolades
4 References
5 External links
Synopsis[edit]
Two years after the success of Oliver Twist, Charles Dickens (Dan Stevens) is suffering financial hardship from the failure of his last three books. Rejected by his publishers, he sets out to write a new book to restore his finances. Seeing inspiration around London, most notably a rich man's funeral that is largely unattended, he begins writing A Christmas Carol, due in six weeks in order to be published by Christmas. As Charles begins to develop his story, he interacts with the characters he is writing about, most notably Ebenezer Scrooge (Christopher Plummer). Helping Dickens is one of his servants, Tara, an Irish immigrant who is literate and able to provide advice.
While writing his book, Charles is greeted by the arrival of his father, John Dickens (Jonathan Pryce), who views him as immature and fiscally irresponsible. Charles's relationship with his family is increasingly strained as he struggles to finish the book in time, as he is unable to resolve Scrooge's story. Hearing that Charles intends to let Tiny Tim die, Tara suggests a resolution for Scrooge by having him save Tiny Tim instead. Charles rejects her help, and soon sends her away from his house in a fit of rage. Additionally, Charles has a falling out with his father and sends him away upon learning that he has been selling Charles's signature.
It is revealed that much of Charles's animosity towards his father is from his childhood embarrassment of working in a blacking factory after his family was taken to debtor's prison. Returning to the long-abandoned factory, Charles is forced to confront his own insecurities through Scrooge. Charles realizes that his story should be one of redemption, and races home to finish his manuscript. As he leaves to submit it to his illustrator, he encounters Tara, and invites her back. His wife suggests he do the same with his father, who is about to board a train to leave London. Reconnecting with his family, Charles submits the manuscript in time for publishing before Christmas. The film ends with the Dickens family celebrating the holidays, while a title text explains the overnight success of A Christmas Carol, and its lasting impact on the Christmas holiday.
Cast[edit]
Dan Stevens as Charles Dickens
Ely Solan as young Charles
Christopher Plummer as Ebenezer Scrooge
Jonathan Pryce as John Dickens, Charles Dickens' father
Simon Callow as John Leech, an illustrator
Donald Sumpter as Jacob Marley
Miriam Margolyes as Mrs. Fisk
Morfydd Clark as Kate Dickens
Justin Edwards as John Forster/Ghost of Christmas Present
Miles Jupp as William Makepeace Thackeray
Ian McNeice as Edward Chapman
Bill Paterson as Mr. Grimsby
John Henshaw as Mr. Fezziwig
Annette Badland as Mrs. Fezziwig
Anna Murphy as Tara/Ghost of Christmas Past
Jasper Hughes-Cotter as Walter Dickens
Eddie Jackson as Scam Artist
Neil Slevin as Italian Workman
Paul Kealyn as Warren's Foreman
Aleah Lennon as Mamie Dickens
Ger Ryan as Elizabeth Dickens
Valeria Bandino as Tart
Release[edit]
The film was released in the United States in 500 theaters on 22 November 2017.[6]
Critical response[edit]
On review aggregator website Rotten Tomatoes, the film has an approval rating of 80% based on 149 reviews, with an average rating of 6/10. The site's critical consensus reads, "The Man Who Invented Christmas adds holiday magic to the writing of A Christmas Carol, putting a sweetly revisionist spin on the story behind a classic yuletide tale."[7] On Metacritic, which assigns a normalized rating to reviews, the film has a weighted average score 60 out of 100, based 32 critics, indicating "mixed or average reviews".[8]
Accolades[edit]
Award
Date of ceremony
Category
Recipient(s) and nominee(s)
Result
Ref.
Saturn Awards
June 2018 Best International Film The Man Who Invented Christmas Pending [9]
References[edit]
Jump up ^ "Opening Gala: The Man Who Invented Christmas". 2017. Retrieved 20 November 2017.
Jump up ^ "THE MAN WHO INVENTED CHRISTMAS (PG)". British Board of Film Classification. Retrieved October 22, 2017.
Jump up ^ "The Man Who Invented Christmas (2017)". Box Office Mojo. Retrieved 24 January 2018.
Jump up ^ Hipes, Patrick. "Dan Stevens & Christopher Plummer To Star In Charles Dickens Tale 'The Man Who Invented Christmas'". Deadline Hollywood. Deadline Hollywood. Retrieved 10 November 2016.
Jump up ^ "The Man Who Invented Christmas UK Release Date Announced - Filmoria". www.filmoria.co.uk. Retrieved 2018-01-08.
Jump up ^ D'Alessandro, Anthony (20 November 2017). "Can 'Coco' Whip 'Justice League' For Top Spot Over Thanksgiving Stretch? – Box Office Preview". Deadline.com. Retrieved 20 November 2017.
Jump up ^ "The Man Who Invented Christmas (2017)". Rotten Tomatoes. Retrieved 29 November 2017.
Jump up ^ "The Man Who Invented Christmas reviews". Metacritic. Retrieved 29 November 2017.
Jump up ^ McNary, Dave (March 15, 2018). "'Black Panther,' 'Walking Dead' Rule Saturn Awards Nominations". Variety. Archived from the original on March 15, 2018. Retrieved March 15, 2018.
External links[edit]
The Man Who Invented Christmas on IMDb
Official website
[show]
v
t
e
Films directed by Bharat Nalluri
Downtime (1997)
Killing Time (1998)
The Crow: Salvation (2000)
Tsunami: The Aftermath (2006)
Miss Pettigrew Lives for a Day (2008)
Spooks: The Greater Good (2015)
The Man Who Invented Christmas (2017)
[show]
v
t
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Bibliography
Novels
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Bleak House
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Household Words
All the Year Round
Collaborations
"A House to Let"
"The Haunted House"
"A Message from the Sea"
"Mugby Junction"
No Thoroughfare
See also
Catherine Dickens (wife)
Epitaph of Charles Irving Thornton
Bleak House
Dickens and Little Nell (statue)
Dickens of London (1976 miniseries)
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Dickensian (2015 TV series)
The Man Who Invented Christmas (2017 film)
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Charles Dickens's A Christmas Carol
Characters
Ebenezer Scrooge
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A Christmas Carol (1908)
A Christmas Carol (1910)
Scrooge (1913)
Scrooge (1935)
A Christmas Carol (1938)
Scrooge (1951)
It's Never Too Late
A Christmas Carol (1960)
Scrooge (1970)
A Christmas Carol (1971)
An American Christmas Carol
Mickey's Christmas Carol
Scrooged
The Muppet Christmas Carol
A Christmas Carol (1997)
A Diva's Christmas Carol
Christmas Carol: The Movie
A Carol Christmas
Springtime with Roo
Chasing Christmas
A Christmas Carol (2006)
A Dennis the Menace Christmas
An American Carol
Ghosts of Girlfriends Past
A Christmas Carol (2009)
The Smurfs: A Christmas Carol (2011)
Television
"The Christmas Carol" (1949)
A Christmas Carol (1954)
Mister Magoo's Christmas Carol
A Carol for Another Christmas
Rich Little's Christmas Carol
A Special Sesame Street Christmas
The Stingiest Man in Town
Bugs Bunny's Christmas Carol
A Christmas Carol (1982)
A Christmas Carol (1984)
Blackadder's Christmas Carol
A Flintstones Christmas Carol
Ebbie
Ebenezer
An All Dogs Christmas Carol
A Christmas Carol (1999)
A Christmas Carol (2000)
An Easter Carol
A Christmas Carol (2004)
Karroll's Christmas
Bah, Humduck! A Looney Tunes Christmas
Nan's Christmas Carol
"A Christmas Carol" (Doctor Who)
It's Christmas, Carol!
Kelly Clarkson's Cautionary Christmas Music Tale
Musicals
Scrooge (1992)
A Christmas Carol (1994)
Mrs. Bob Cratchit's Wild Christmas Binge (2002)
Plays
A Christmas Carol (1988)
Fellow Passengers (2004)
A Klingon Christmas Carol (2007)
Soundtracks
A Christmas Carol (2009)
Doctor Who: A Christmas Carol (2011)
Other
Adaptations of A Christmas Carol
Batman: Noël (comic)
"Green Christmas" (single)
The Misadventures of the Wholesome Twins
The Man Who Invented Christmas

This 2010s drama film–related article is a stub. You can help Wikipedia by expanding it.
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Retrieved from "https://en.wikipedia.org/w/index.php?title=The_Man_Who_Invented_Christmas_(film)&oldid=831953778"
Categories:
2017 films
English-language films
Bleecker Street films
Films directed by Bharat Nalluri
Films set in 1843
Cultural depictions of Charles Dickens
Films about writers
Works about Charles Dickens
2010s drama films
Irish films
Canadian Christmas films
Canadian films
2010s drama film stubs
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values: مردی که کریسمس را اختراع کرد – Persian

values: 찰스 디킨스의 비밀 서재 – Korean

values: The Man Who Invented Christmas – Indonesian

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